Podcasts about Spectrometer

MSOLO will head back to the Moon to search for gases trapped beneath the lunar surface.

Many farmers have readily adopted high-tech ways of growing their crops.

Today in Lighting is brought to you by Amerlux, producers of the new Grid Cove series. Learn more. Highlights today include: Elemental LED Acquires Gammalux Lighting Systems, DALI Alliance Expands Board of Directors to Support Global Growth and Innovation, Lightovation to Hold NAILD Controls Certification Program, Electrical Trends: Overcoming Online Pricing Challenges in B2B eCommerce, Sekonic Unveils C-4000 Spectrometer.

The ScienceCraft for Outer Planet Exploration, or SCOPE, cleverly combines a science instrument with the spacecraft itself.

In your Phone Tap Brooke calls a guy who recently checked out a movie from the library to accuse him of leaving some…. Traces… all over her precious books!See omnystudio.com/listener for privacy information.

In your Phone Tap Brooke calls a guy who recently checked out a movie from the library to accuse him of leaving some…. Traces… all over her precious books!See omnystudio.com/listener for privacy information.

More mailbag! A look at the RadiaCode Radiation Monitor, and the LattePanda Mu Intel N100 Compute Module. https://www.radiacode.com/ https://amzn.to/3yV5Gp4 https://www.lattepanda.com/lattepanda-mu https://www.dfrobot.com/kit-004.html Github: https://github.com/LattePandaTeam/LattePanda-Mu/tree/main/Electricals/Examples/%5BDFR1141%5DFull%20EVA%20Carrier%20for%20LattePanda%20Mu Part 2: https://www.youtube.com/watch?v=UE_srZZdPjM 00:00 – Mailbag 00:30 – Radiacode 103 Radiation Detector & Spectrometer 07:48 – Teardown 14:09 – LattePanda Mu Intel N100 Compute Module 25:22 – Power up Forum: https://www.eevblog.com/forum/blog/eevblog-1621-mailbag-radiacode-radiation-monitor-lattepanda-mu-compute-modu/

The OGS, the Optical Gas Spectrometer, is a feat of engineering. In the previous episode, we discussed what it can do and how it works. Today, Bosch associate and OGS inventor Alex Stratmann talks more about turning Raman spectrometers into an industrial product. Many considerations had to be made, from the custom laser source to the material used for the seals, and we also learn that OGS development hasn't stopped: The team is working on a high-pressure version and on efforts to measure almost any gas in the world. More Bosch podcasts: Previous episode: https://fromknowhowtowow.podigee.io/65-optical-gas-spectrometer Beyond Bosch: https://podtail.com/de/podcast/beyond-bosch/

Take a deep breath. What you just breathed in was probably about 78% nitrogen and 21% oxygen and some minor other components. But how do you measure that? Measuring gases and their concentrations has been pretty difficult, says Bosch physicist Alex Stratmann. His team's invention, the optical gas spectrometer, OGS, is set to change that. It packs what used to be a complex lab setup into a tabletop device. OGS leverages Raman spectroscopy, a method that exists for about a 100 years and has been used e.g. in the art world to analyze pigments. Our hosts Melena and Shuko learn from Cristina Aibéo, a chemist at Berlin's National Museums, how Raman spectroscopy can help solve crimes and also save energy. At Bosch, on the other hand, the OGS helps with measuring hydrogen - and thus with the transition to a green hydrogen economy. Breathe in, breathe out, hit play! From Know-how to Wow”: How to produce green hydrogen? https://www.youtube.com/watch?v=fvbHOY7GAig

Join us on H2TechTalk, the leading podcast for sustainable energy enthusiasts, as we delve into the groundbreaking technology behind Bosch's Optical Gas Spectrometer (OGS). In this episode, we sit down with Franziska Seitz, Product Manager, and Annika Reiser, Key Account Manager, from Robert Bosch GmbH to explore the OGS's role in revolutionizing the hydrogen industry. Discover how this innovative device, based on Raman spectroscopy, provides real-time insights into gas composition, enabling precise control over various applications. Don't miss out on this exclusive look at Bosch's OGS, a game-changer in the world of hydrogen innovation. Subscribe now to stay connected with the latest in sustainable solutions! Links discussed in this episode: Video on the OGS - https://media.video.bosch.com/media/OGS_Video_H2/0_jdx88k0u OGS Graphic - https://www.bosch-ibusiness.com/media/images/products/sensors/xx_pdfs_1/ogs_introduction_short.pdf#page=13 Bosch website - https://www.bosch-ibusiness.com/products/sensors/ For more information regarding Bosch's OGS, please contact contact.ogs@de.bosch.com

The CO 2 Profile and Analytical Model for the Pioneer Venus Large Probe Neutral Mass Spectrometer by Rakesh Mogul et al. on Thursday 24 November We present a significantly updated CO$_2$ altitude profile for Venus (64.2-0.9 km) and provide support for a potential deep lower atmospheric haze of particles (17 km and lower). We extracted this information by developing a new analytical model for mass spectra obtained by the Pioneer Venus Large Probe (PVLP) Neutral Mass Spectrometer (LNMS). Our model accounts for changes in LNMS configuration and output during descent and enables the disentanglement of isobaric species via a data fitting routine that adjusts for mass-dependent changes in peak shape. The model yields CO$_2$ in units of density (kg m-3), isotope ratios for $^{13}$C/$^{12}$C and $^{18}$O/$^{16}$O, and 14 measures of CO$_2$ density across 55.4-0.9 km, which represents the most complete altitude profile for CO$_2$ at 60 km towards the surface to date. The CO$_2$ density profile is also consistent with the pressure, temperature, and volumetric gas measurements from the PVLP and VeNeRa spacecraft. Nominal and low-noise operations for the LNMS mass analyzer are supported by the behaviors (e.g., ionization yields, fragmentation yields, and peak shapes) of several internal standards (e.g., CH$^{3+}$, CH$^{4+}$, $^{40}$Ar$^+$, $^{136}$Xe$^{2+}$, and $^{136}$Xe$^+$), which were tracked across the descent. Lastly, our review of the CO$_2$ profile and LNMS spectra reveals hitherto unreported partial and rapidly clearing clogs of the inlet in the lower atmosphere, along with several ensuing data spikes at multiple masses. Together, these observations suggest that atmospheric intake was impacted by particles at 17 km (and lower) and that rapid particle degradation at the inlet yielded a temporary influx of mass signals into the LNMS. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12557v1

The CO 2 Profile and Analytical Model for the Pioneer Venus Large Probe Neutral Mass Spectrometer by Rakesh Mogul et al. on Thursday 24 November We present a significantly updated CO$_2$ altitude profile for Venus (64.2-0.9 km) and provide support for a potential deep lower atmospheric haze of particles (17 km and lower). We extracted this information by developing a new analytical model for mass spectra obtained by the Pioneer Venus Large Probe (PVLP) Neutral Mass Spectrometer (LNMS). Our model accounts for changes in LNMS configuration and output during descent and enables the disentanglement of isobaric species via a data fitting routine that adjusts for mass-dependent changes in peak shape. The model yields CO$_2$ in units of density (kg m-3), isotope ratios for $^{13}$C/$^{12}$C and $^{18}$O/$^{16}$O, and 14 measures of CO$_2$ density across 55.4-0.9 km, which represents the most complete altitude profile for CO$_2$ at 60 km towards the surface to date. The CO$_2$ density profile is also consistent with the pressure, temperature, and volumetric gas measurements from the PVLP and VeNeRa spacecraft. Nominal and low-noise operations for the LNMS mass analyzer are supported by the behaviors (e.g., ionization yields, fragmentation yields, and peak shapes) of several internal standards (e.g., CH$^{3+}$, CH$^{4+}$, $^{40}$Ar$^+$, $^{136}$Xe$^{2+}$, and $^{136}$Xe$^+$), which were tracked across the descent. Lastly, our review of the CO$_2$ profile and LNMS spectra reveals hitherto unreported partial and rapidly clearing clogs of the inlet in the lower atmosphere, along with several ensuing data spikes at multiple masses. Together, these observations suggest that atmospheric intake was impacted by particles at 17 km (and lower) and that rapid particle degradation at the inlet yielded a temporary influx of mass signals into the LNMS. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12557v1

The CO2 Profile and Analytical Model for the Pioneer Venus Large Probe Neutral Mass Spectrometer by Rakesh Mogul et al. on Wednesday 23 November We present a significantly updated CO2 altitude profile for Venus (64.2-0.9 km) and provide support for a potential deep lower atmospheric haze of particles (17 km and lower). We extracted this information by developing a new analytical model for mass spectra obtained by the Pioneer Venus Large Probe (PVLP) Neutral Mass Spectrometer (LNMS). Our model accounts for changes in LNMS configuration and output during descent and enables the disentanglement of isobaric species via a data fitting routine that adjusts for mass-dependent changes in peak shape. The model yields CO2 in units of density (kg m-3), isotope ratios for 13C/12C and 18O/16O, and 14 measures of CO2 density across 55.4-0.9 km, which represents the most complete altitude profile for CO2 at 60 km towards the surface to date. The CO2 density profile is also consistent with the pressure, temperature, and volumetric gas measurements from the PVLP and VeNeRa spacecraft. Nominal and low-noise operations for the LNMS mass analyzer are supported by the behaviors (e.g., ionization yields, fragmentation yields, and peak shapes) of several internal standards (e.g., CH3+, CH4+, 40Ar+, 136Xe2+, and 136Xe+), which were tracked across the descent. Lastly, our review of the CO2 profile and LNMS spectra reveals hitherto unreported partial and rapidly clearing clogs of the inlet in the lower atmosphere, along with several ensuing data spikes at multiple masses. Together, these observations suggest that atmospheric intake was impacted by particles at 17 km (and lower) and that rapid particle degradation at the inlet yielded a temporary influx of mass signals into the LNMS. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12557v1

The CO 2 Profile and Analytical Model for the Pioneer Venus Large Probe Neutral Mass Spectrometer by Rakesh Mogul et al. on Wednesday 23 November We present a significantly updated CO$_2$ altitude profile for Venus (64.2-0.9 km) and provide support for a potential deep lower atmospheric haze of particles (17 km and lower). We extracted this information by developing a new analytical model for mass spectra obtained by the Pioneer Venus Large Probe (PVLP) Neutral Mass Spectrometer (LNMS). Our model accounts for changes in LNMS configuration and output during descent and enables the disentanglement of isobaric species via a data fitting routine that adjusts for mass-dependent changes in peak shape. The model yields CO$_2$ in units of density (kg m-3), isotope ratios for $^{13}$C/$^{12}$C and $^{18}$O/$^{16}$O, and 14 measures of CO$_2$ density across 55.4-0.9 km, which represents the most complete altitude profile for CO$_2$ at 60 km towards the surface to date. The CO$_2$ density profile is also consistent with the pressure, temperature, and volumetric gas measurements from the PVLP and VeNeRa spacecraft. Nominal and low-noise operations for the LNMS mass analyzer are supported by the behaviors (e.g., ionization yields, fragmentation yields, and peak shapes) of several internal standards (e.g., CH$^{3+}$, CH$^{4+}$, $^{40}$Ar$^+$, $^{136}$Xe$^{2+}$, and $^{136}$Xe$^+$), which were tracked across the descent. Lastly, our review of the CO$_2$ profile and LNMS spectra reveals hitherto unreported partial and rapidly clearing clogs of the inlet in the lower atmosphere, along with several ensuing data spikes at multiple masses. Together, these observations suggest that atmospheric intake was impacted by particles at 17 km (and lower) and that rapid particle degradation at the inlet yielded a temporary influx of mass signals into the LNMS. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12557v1

The CO2 Profile and Analytical Model for the Pioneer Venus Large Probe Neutral Mass Spectrometer by Rakesh Mogul et al. on Wednesday 23 November We present a significantly updated CO2 altitude profile for Venus (64.2-0.9 km) and provide support for a potential deep lower atmospheric haze of particles (17 km and lower). We extracted this information by developing a new analytical model for mass spectra obtained by the Pioneer Venus Large Probe (PVLP) Neutral Mass Spectrometer (LNMS). Our model accounts for changes in LNMS configuration and output during descent and enables the disentanglement of isobaric species via a data fitting routine that adjusts for mass-dependent changes in peak shape. The model yields CO2 in units of density (kg m-3), isotope ratios for 13C/12C and 18O/16O, and 14 measures of CO2 density across 55.4-0.9 km, which represents the most complete altitude profile for CO2 at 60 km towards the surface to date. The CO2 density profile is also consistent with the pressure, temperature, and volumetric gas measurements from the PVLP and VeNeRa spacecraft. Nominal and low-noise operations for the LNMS mass analyzer are supported by the behaviors (e.g., ionization yields, fragmentation yields, and peak shapes) of several internal standards (e.g., CH3+, CH4+, 40Ar+, 136Xe2+, and 136Xe+), which were tracked across the descent. Lastly, our review of the CO2 profile and LNMS spectra reveals hitherto unreported partial and rapidly clearing clogs of the inlet in the lower atmosphere, along with several ensuing data spikes at multiple masses. Together, these observations suggest that atmospheric intake was impacted by particles at 17 km (and lower) and that rapid particle degradation at the inlet yielded a temporary influx of mass signals into the LNMS. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12557v1

The CO 2 Profile and Analytical Model for the Pioneer Venus Large Probe Neutral Mass Spectrometer by Rakesh Mogul et al. on Wednesday 23 November We present a significantly updated CO$_2$ altitude profile for Venus (64.2-0.9 km) and provide support for a potential deep lower atmospheric haze of particles (17 km and lower). We extracted this information by developing a new analytical model for mass spectra obtained by the Pioneer Venus Large Probe (PVLP) Neutral Mass Spectrometer (LNMS). Our model accounts for changes in LNMS configuration and output during descent and enables the disentanglement of isobaric species via a data fitting routine that adjusts for mass-dependent changes in peak shape. The model yields CO$_2$ in units of density (kg m-3), isotope ratios for $^{13}$C/$^{12}$C and $^{18}$O/$^{16}$O, and 14 measures of CO$_2$ density across 55.4-0.9 km, which represents the most complete altitude profile for CO$_2$ at 60 km towards the surface to date. The CO$_2$ density profile is also consistent with the pressure, temperature, and volumetric gas measurements from the PVLP and VeNeRa spacecraft. Nominal and low-noise operations for the LNMS mass analyzer are supported by the behaviors (e.g., ionization yields, fragmentation yields, and peak shapes) of several internal standards (e.g., CH$^{3+}$, CH$^{4+}$, $^{40}$Ar$^+$, $^{136}$Xe$^{2+}$, and $^{136}$Xe$^+$), which were tracked across the descent. Lastly, our review of the CO$_2$ profile and LNMS spectra reveals hitherto unreported partial and rapidly clearing clogs of the inlet in the lower atmosphere, along with several ensuing data spikes at multiple masses. Together, these observations suggest that atmospheric intake was impacted by particles at 17 km (and lower) and that rapid particle degradation at the inlet yielded a temporary influx of mass signals into the LNMS. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12557v1

Inconspicuous Solar Polar Coronal X-ray Jets as the Source of Conspicuous Hinode EUV Imaging Spectrometer EIS Doppler Outflows by Alphonse C. Sterling et al. on Tuesday 18 October We examine in greater detail five events previously identified as being sources of strong transient coronal outflows in a solar polar region in Hinode/EUV Imaging Spectrometer (EIS) Doppler data. Although relatively compact or faint and inconspicuous in Hinode/Soft X-ray Telescope (XRT) soft-X-ray (SXR) images and in Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) EUV images, we find that all of these events are consistent with being faint coronal X-ray jets. The evidence for this is that the events result from eruption of minifilaments of projected sizes spanning 5000 -- 14,000 km and with erupting velocities spanning 19 -- 46 km/s, which are in the range of values observed in cases of confirmed X-ray polar coronal hole jets. In SXR images, and in some EUV images, all five events show base brightenings, and faint indications of a jet spire that (in four of five cases where determinable) moves away from the brightest base brightening; these properties are common to more obvious X-ray jets. For a comparatively low-latitude event, the minifilament erupts from near (

Inconspicuous Solar Polar Coronal X-ray Jets as the Source of Conspicuous Hinode EUV Imaging Spectrometer EIS Doppler Outflows by Alphonse C. Sterling et al. on Tuesday 18 October We examine in greater detail five events previously identified as being sources of strong transient coronal outflows in a solar polar region in Hinode/EUV Imaging Spectrometer (EIS) Doppler data. Although relatively compact or faint and inconspicuous in Hinode/Soft X-ray Telescope (XRT) soft-X-ray (SXR) images and in Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) EUV images, we find that all of these events are consistent with being faint coronal X-ray jets. The evidence for this is that the events result from eruption of minifilaments of projected sizes spanning 5000 -- 14,000 km and with erupting velocities spanning 19 -- 46 km/s, which are in the range of values observed in cases of confirmed X-ray polar coronal hole jets. In SXR images, and in some EUV images, all five events show base brightenings, and faint indications of a jet spire that (in four of five cases where determinable) moves away from the brightest base brightening; these properties are common to more obvious X-ray jets. For a comparatively low-latitude event, the minifilament erupts from near (

A horn-coupled millimeter-wave on-chip spectrometer based on Lumped Element Kinetic Inductance Detectors by Usasi Chowdhury et al. on Tuesday 06 September Context. Millimetre-wave astronomy is an important tool for both general astrophysics studies and cosmology. A large number of unidentified sources are being detected by the large field-of-view continuum instruments operating on large telescopes. Aims. New smart focal planes are needed to bridge the gap between large bandwidth continuum instruments operating on single dish telescopes and the high spectral and angular resolution interferometers (e.g. ALMA in Chile, NOEMA in France). The aim is to perform low-medium spectral resolution observations and select a lower number of potentially interesting sources, i.e. high-redshift galaxies, for further follow-up. Methods. We have designed, fabricated and tested an innovative on-chip spectrometer sensitive in the 85-110~GHz range. It contains sixteen channels selecting a frequency band of about 0.2 GHz each. A conical horn antenna coupled to a slot in the ground plane collects the radiation and guides it to a mm-wave microstrip transmission line placed on the other side of the mono-crystalline substrate. The mm-wave line is coupled to a filter-bank. Each filter is capacitively coupled to a Lumped Element Kinetic Inductance Detector (LEKID). The microstrip configuration allows to benefit from the high quality, i.e. low losses, mono-crystalline substrate, and at the same time prevents direct, i.e. un-filtered, LEKID illumination. Results. The prototype spectrometer exhibit a spectral resolution R = lambda / Delta_lambda = 300. The optical noise equivalent power is in the low 1E-16W/sqrt(Hz) range for an incoming power of about 0.2pW per channel. The device is polarisation-sensitive, with a cross-polarisation lower than 1% for the best channels. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.02484v1

Dr Bryan Ardis is a man on a mission to put these White Coated criminals where they belong, and to warn people of the dangers posed by media and political pressures to get jabbed. He's recently received results from a blood clot he gave to Mike Adams to do mass spec analysis. He shares the findings with me on this Ba'al Busters episode. The conversation later leads me to an opportunity to ask him a tough question about the nature of SIDS, and you'll be shocked and appalled to hear the answer. Please, if SIDS has affected your family, I viewer discretion is advised. You will be angry to learn how they took your child or your sibling away from you. https://theDrArdisShow.com for more!VISIT https://GiveSendGo.com/BaalBusters and be on the right side of history. Defend Your Rights, Support Independent Media! https://www.tipeeestream.com/baal-busters/donationor https://paypal.me/BaalBusters Support Those Whom Support FreedomBA'AL BUSTERS shirts and merch https://my-store-c960b1.creator-spring.com/ADD My FREE RokuTV Baal Busters Channel here:https://channelstore.roku.com/details/a44cff88b32c2fcc7e090320c66c4d09/baal-busters-broadcast

COR is an infrared spectrometer that measures your blood health and how the food you eat and the exercise that you engage in impacts it. The first product of its kind, COR was created by a former Apple Health exec who wanted to know: is my diet good for me? Because everyone's response -- even to theoretically healthy foods -- is different. Even genetically identical twins don't have the same metabolic response to things, recent studies have shown. So the idea with COR is that you analyze your blood at home via infrared spectrometry about 4 times over a 3-week period, and you get specific data and recommendations back about what's good -- and what's bad -- for your health. The result, CEO Bob Messerschmidt says, is potentially the ability to have another 15 years of healthy, productive life. Links: Support TechFirst with $SMRT coins: https://rally.io/creator/SMRT/ Buy $SMRT to join a community focused on tech for good: the emerging world of smart matter. Access my private Slack, get your name in my book, suggest speakers for TechFirst ... and support my work. TechFirst transcripts: https://johnkoetsier.com/category/tech-first/ Forbes columns: https://www.forbes.com/sites/johnkoetsier/ Full videos: https://www.youtube.com/c/johnkoetsier?sub_confirmation=1 Keep in touch: https://twitter.com/johnkoetsier

Welcome to another Episode of Marijuana SA Weekly. Thanks for Listening guys!

Students in MIT's course 5.310 Laboratory Chemistry have a state-of-the art lab to work in, with energy-saving hibernating fume hoods and a new spectrometer that achieves mind-blowingly precise measurements—not parts per million or parts per billion, but parts per trillion! And the students do spend much of their time in that new lab. But Dr. John Dolhun, director of the Undergraduate Chemistry Teaching Labs at MIT, who taught 5.310 for many years, and Dr. Sarah Hewett, who currently teaches it, make sure that the course doesn't take place entirely behind closed doors. One of the lab activities involves collecting water samples from the Charles River and analyzing them for dissolved oxygen and contaminants such as phosphates. This activity, named the “Ellen Swallow Richards Lab” after an environmental chemist who was also the first female student at MIT, ensures that the coursework is grounded in real-world concerns. In this episode, Dr. Dolhun and Dr. Hewett discuss that lab and other topics, such as how to teach perseverance, why their course emphasizes ways of communicating science to an audience of nonscientists, and the importance of sharing educational resources. Relevant ResourcesMIT OpenCourseWareThe OCW Educator PortalShare your teaching ideas and insights with John Dolhun and Sarah HewettDr. Dolhun and Dr. Hewett's course on OCWChemLab Boot Camp video series on OCWEllen Swallow Richards biography at WikipediaMIT Spectrum article on the new undergraduate chemistry labsMIT News article on energy-saving measures in the undergraduate chemistry labsMusic in this episode by Blue Dot Sessions Connect with UsIf you have a suggestion for a new episode or have used OCW to change your life or those of others, tell us your story. We'd love to hear from you! Call us @ 617-715-2517On our siteOn FacebookOn TwitterOn Instagram Stay CurrentSubscribe to the free monthly "MIT OpenCourseWare Update" e-newsletter. Support OCWIf you like Chalk Radio and OpenCourseware, please donate to help keep those programs going! CreditsSarah Hansen, host and producer Brett Paci, producer  Dave Lishansky, producer Script writing assistance by Aubrey CalawayShow notes by Peter Chipman

In pharma, the use of gas analysis in fermentation bioreactors is critical for monitoring the health of a culture, and measuring small changes to oxygen and carbon dioxide concentrations at key phases of the process. Whether using continuous or batch fermentation for bacterial, microbial or mammalian cell culture expression, Thermo Fischer Scientific's gas analysis mass spectrometry product range provides precise off-gas analysis through every stage of fermentation. To learn more about the Prima BT and Prima PRO models, senior editor Meagan Parrish chats with Daniel Merriman, strategic marketing manager, Thermo Fischer. Read the transcript: https://www.pharmamanufacturing.com/podcasts/off-script-a-pharma-manufacturing-podcast/solutions-spotlight-gas-analysis-mass-spectrometer-applications-in-fermentation-and-cell-culture-process

Macquarie University's Doctor Christian Schwab developed a new kind of spectrometer that brings solar systems into sharper focus to aid in the discovery of smaller exoplanets. On this episode, we learn more about NEID. The post Tuning In To Exoplanets : A New Spectrometer Aims To Find More Planets Out There appeared first on Trekzone.

Welcome to the first episode of Matt Spectro thru the Multiverse. On this very special first episode my brother Travis joins the Multiverse as we look back at the one that started it all! We go back to 1941 watch Superman vs The Mad Scientist and give our thoughts. Has Superman changed over the years?!?  How will we rank it on the Spectrometer?!?  Lets find out together!!!!

1:00? What made you excited about the shuttle? 2:22? The spectrometer design - radar signal processing 4:00? built in self test 4:18? in & output signals 6:00? design in Chisel 10:40? ASIC vs FPGA 11:30? showing the GDS 12:24? density of the design 13:30? contact details https://github.com/milovanovic/spectr...? https://www.zerotoasic.com/?

NASA is planning to send a mobile robot to the South Pole of the Moon to get a close-up view of water ice.

IN THIS EPISODE I SHARE SOME FACTS ON THE INVENTOR GEORGE ALCORN. GEORGE ALCORN INVENTED THE X RAY SPECTROMETER AND PATENTED THE TECHNOLOGY. HIS INVENTION HAS LED TO DEEPER DISCOVERY OF OUR UNIVERSE AND PAVED THE WAY FOR MANY MORE INVENTIONS. I HAD THE OPPORTUNITY TO MEET HIM WHEN HE WAS INDUCTED INTO THE INVENTORS HALL OF FAME IN 2015. HIS INVENTIONS HAVE IMPACTED THE SCIENCE OF PHYSICS AND AEROSPACE. https://en.wikipedia.org/wiki/George_Edward_Alcorn_Jr. https://www.invent.org/inductees/george-edward-alcorn NASA HALL OF FAME INVENTORS NASA HALL OF FAME BLACK AMERICAN SCIENTISTS AMERICAN SCIENTISTS AFRICAN AMERICAN SCIENTISTS NASA SCIENTIST HALL OF FAME INVENTORS PATENTED INVENTIONS INVENTIONS THAT CHANGED THE WORLD SCIENCE IN HISTORY LIVING LEGEND PHYSICS PHD IN SCIENCE AEROSPACE INVENTOR INVENTORS INNOVATORS SCIENCE PODCAST INTERESTING FACTS PODCAST HISTORY PODCAST Topics revolve around society & culture, product reviews, science & tech, history, money matters, business, health & fitness, entertainment. Occasional movie reviews and a few random topics just for fun all delivered in a casual tell it like it is manner. Delivering solo episodes, conversations, and interviews. https://howtheydiditandwhy.com/ .https://www.youtube.com/channel/UCpxmXHQP63G_OxjV9MH-1jQ https://podcasts.apple.com/us/podcast/how-they-did-it-and-why/id1535893420 https://open.spotify.com/show/6ZiFFBsxDPaqW9sJcoQdtj https://www.stitcher.com/podcast/how-they-did-it-and-why https://www.instagram.com/how_they_did_it_and_why/ https://howtheydiditandwhy.blogspot.com/ https://www.facebook.com/How-they-did-it-and-why-127403185762180 https://podcasts.google.com/feed/aHR0cHM6Ly9mZWVkcy5yZWRjaXJjbGUuY29tLzcxY2Q4OTgxLTY0NGItNDg5Ni1hZDM5LTVjNThjNmQ1N2ExNg== https://music.amazon.com/podcasts/30b86c32-9e38-47a3-bd54-0d6aacdc7eb9/HOW-THEY-DID-IT-AND-WHY https://www.pandora.com/podcast/how-they-did-it-and-why/PC:51915?part=PC:51915&corr=podcast_organic_external_site&TID=Brand:POC:PC51915:podcast_organic_external_site https://radiopublic.com/how-they-did-it-and-why-GEoY94 https://www.stitcher.com/show/how-they-did-it-and-why https://www.pinterest.com/andwhypodcast/how-they-did-it-and-why-podcast-society-more/ https://music.amazon.com/podcasts/30b86c32-9e38-47a3-bd54-0d6aacdc7eb9/HOW-THEY-DID-IT-AND-WHY https://www.pandora.com/podcast/how-they-did-it-and-why/PC:51915?part=PC:51915&corr=podcast_organic_external_site&TID=Brand:POC:PC51915:podcast_organic_external_site The goal here is to learn from others experiences. If your an entrepreneur, on a path of self discovery and inspired by the significant achievements of others you might find this podcast a good fit. Topics revolve around society & culture, product reviews, science & tech, history, money matters, business, health & fitness, entertainment. Occasional movie reviews and a few random topics just for fun all delivered in a casual tell it like it is manner. Delivering solo episodes, conversations, and interviews. RANDOM FACTS MOTIVATION CARRER GOALS INTERVIEWS INDUSTRY INTERVIEWS OPINION HOW TO PRODUCT REVIEWS FOOD REVIEWS SNACK REVIEWS HEALTH FITNESS SCIENCE FACTS list25 science facts list weird weird science bizarre science science facts facts about science crazy facts weird facts bizarre facts strange facts strange science facts interesting education interesting facts incredible science facts 25 weird science facts you may not know 25 facts strange science interesting science interesting science facts INTERESTING HEALTH FACTS SELF CARE MENTAL HEALTH BUSINESS MOTIVATION SMALL BUSINESS Entrepreneur BUSINESS REVIEWS TECH REVIEWS HEALTHY FOOD LIFE HACKS AMAZON PRODUCT REVIEWS AMAZON REVIEWS BEST OF AMAZON AMAZON MUST HAVE PRODUCTS MOVIE REVIEWS LEARN HISTORY FACTS HISTORY AND SCIENCE HISTORICAL FIGURES psychological facts psychology facts psychology 101 human behavior psychology tricks that work on anybody how to persuade topthink SOCIETY & CULTURE psychology facts brainy dose BUDGET SIDE HUSSLES SAVE MONEY MONEY MANAGEMENT TIME MANAGEMENT HEALTH FACTS how to make extra income money ideas how to make extra money business videos how to start a business small business ideas hair business hair extensions business hair extensions company side hustles 20 side hustles top 20 side hustles how to make more money online side hustles easy side jobs to make extra money how to make extra money from home side hustles for students law of attraction BUSINESS PODCAST RANDOM FACTS PODCAST HEALTH PODCAST INTERESTING FACTS PODCAST NEW PODCAST THINGS YOU SHOULD KNOW HAIR CARE REVIEWS SKIN CARE REVIEWS DEVICE REVIEWS WOMEN IN HISTORY APP REVIEWS PLATFORM REVIEWS NEW PODCAST NEW YOUTUBE channel New youtube channels Podcast guest Be a podcast guest Be on a podcast GEEK PODCAST NERD PODCAST PODCASTS FOR NERDS PODCASTS FOR GEEKS

I've always wanted a Star Trek tricorder ... a mobile sensor unit that tells you all about the world around you. (Who doesn't?) Now a company in Germany, Trinamix, has partnered with Qualcomm to deliver mobile spectroscopy in mobile phones. No attachments required. All onboard your smartphone. The first applications are in skin care and cosmetics, but the tech can also sense what is on your plate to help you record your diet, or tell you the composition of just about anything around you. In this edition of TechFirst with John Koetsier, we chat with Dr. Wilfried Hermes, the director of IR sensing for Trinamix.

This session will serve as an introduction to a 4 part series in which Dr. Hayden will invite attendees to witness in real time his journey bringing mass spec testing to a clinical lab. During these interactive sessions, attendees will be encouraged to help troubleshoot, and offer advice as desired.Subsequent sessions anticipated include:1. Getting going with mass spectrometry: Josh learns chromatography2. Getting going with mass spectrometry: Josh tries to do sample preparation3. Getting going with mass spectrometry: Josh analyzes peaks

He built a mass spectrometer from scratch and reinvented it in the process!Bearing a smile, Mazdak “Maz” Taghioskoui says he immigrated to the United States from Iran for a good education and same-day shipping, two key features that have supported his focus on building – from scratch – a sophisticated next-generation analytical tool: the Trace Matters SPion mass spectrometer.Maz is the Founder and CEO/CTO of Trace Matters, and we sat down with him for show-and-tell to discuss how he and his company is reinventing the mass spectrometer to save lives here on Earth and to advance our scientific understanding of the cosmos beyond our planet.Show NotesEpisode page, transcript, and podcast listening links: https://toughtechtoday.com/bootstrapping-mass-spectrometry/Mazdak on LinkedIn: https://www.linkedin.com/in/mazdakoskui/Trace Matters (company): https://www.tracematters.com/Greentown Labs (workspace): https://greentownlabs.com/Harvard’s Rapid Acceleration of Diagnostics (RADx): https://www.nejm.org/doi/full/10.1056/NEJMsr2022263Subscribe with your favorite podcast service: https://www.buzzsprout.com/1169378/5983345Watch this show on Youtube: https://youtu.be/2wsX9bWqTj4Topic Timecodes00:54 A lesson in high school chemistry03:44 History and benefits of mass spectrometry for space and medical applications04:53 Screening newborn babies’ blood for disease mitigation06:18 Instrumentation Startup: A tiny company in a world of corporates07:15 Creating a mass spectrometer… from scratch08:56 The fallacy of“if your system is complex and it’s working, you don’t change it”10:11 How I built this12:16 A case study in the 10,000 Hour Rule and brute force science13:38 Seeing years of work finally come to fruition17:24 Seeing SPion and the frog18:53 Expediting mass spectrometry-assisted brain surgery23:36 Show-and-tell in Maz’s lab24:48 Inventing a lab-scale fabrication process28:20 Following a vision or a wandering path?30:08 Getting addicted to solving challenges32:01 Immigrating to the United States for a great education and… quick shipping33:26 The resources at Massachusetts’ Greentown Labs34:37 Bootstrapping a scientific instrument company37:32 A shift in how we build instruments?39:36 Who could be first to benefit from next-generation mass spectrometry?40:52 Integrating learnings into a tech roadmap41:23 The Harvard Rapid Acceleration of Diagnostics (RADx) program and COVID-1942:12 Advice to a younger self: persistence, love, and remembering to eatTagstough tech today,jmill,Jonathan Miller,Forrest Meyen,deep tech,hard tech,startup,entrepreneurship,venture capital,tough tech,tough technology,technology,podcast,Mazdak Taghioskoui,Trace Matters,Trace Matters LLC,Mass Spectrometry,SpIon,Spectrometer,Greentown Labs,Green town labs,Maz,NASA Mass Spectrometry,Mass Spec,Mass Spec surgery,NASA,Science,Physics,quadrupole mass spectrometer,how does a mass spectrometer work,how a mass spec works,meyen

Researchers from the Institute of Genomics and Integrative Biology (IGIB) and the National Centre for Disease Control (NCDC) have developed a technique that uses mass spectrometry to detect novel coronavirus (SARS-CoV-2).

Tune into this week’s episode to hear Brian speak with Lieza Danan of Liveritas Biosciences! -A few quick words from LiVeritas: LiVeritas Biosciences unleashes the power of Mass Spectrometry with industry intelligence to advance high-quality drug candidates for our partners to deliver the most optimal clinical outcome for patients. Other mass spectrometry-based startups are grounded in academic theory and academia-developed processes.  At LiVeritas Biosciences, we leverage over 70 years of combined biopharma industry-developed processes, biotech startup lean execution-focused mindset, and clinical diagnostics experience codified into our analytical testing and our SaaS offerings to ensure production of streamlined, high-quality results directly impacting the lives of patients in the clinic.  We are grounded in industry standards as it represents reality. Our collective work improved and saved the real lives of patients in the clinic. Hear about why this company is breaking barriers and the real story behind it all! For more info, please visit https://liveritas.bio/ If you have the next big idea, apply to the Expert Dojo Accelerator: www.expertdojo.com

This is a conversation with Professor David Rothery.David is a professor of planetary geosciences at the Open University where he chairs a level 2 module Planetary Science and the Search for Life. He serves on the Open University's Senate.David worked on the Beagle2 project and in 2006 he was appointed U.K. lead scientist for the MIXS (Mercury Imaging X-ray Spectrometer) on the joint European Space Agency/JAXA mission to Mercury named BepiColombo. He has been a guest several times on The Sky at Night, and has authored numerous science books.In this episode I asked David to give his views and vision on where we might find basic or complex extra-terrestrial life in the galaxy. If we found it, how would we know if it was a second genesis or formed from the same starting point as life on earth. We talked about potential life on icy moons, mars, venus and exoplanets. This conversation covered almost every part of the search for life in space and it was quite stunning to share this time with Professor Rothery, whom I consider to be a learned and informed voice on this subject matter.

Heystek Grobler is an Electronics Engineer and Masters Student that is affiliated with the Hartebeesthoek Radio Astronomy Observatory (HartRAO) which is a facility of the South African Radio Astronomy Observatory (SARAO), as well as the University of Johannesburg (UJ) Department of Electrical and Electronic Engineering Science. He specializes in the field of Digital Signal Processing and has research interests in Spectroscopy and Radiometry. He is currently a part of the Fundamental Astronomy Department at HartRAO where he is developing a new Spectrometer and Radiometer. Heystek is also a member of The Collaboration For Astronomy Signal Processing And Electronics Research (CASPER) Group from the University of Berkeley California (UC Berkeley).

A new NASA-funded planet-hunting instrument has been installed on the WIYN telescope, on Arizona’s Kitt Peak.

A new NASA-funded planet-hunting instrument has been installed on the WIYN telescope, on Arizona’s Kitt Peak.

In this episode Claire Murray explores the other users and developers of instruments like the 'Bragg X-ray spectrometer, England, 1910-1926', including scientists such as Kathleen Lonsdale. We discuss the pioneering work of these scientists in the field, Lonsdale career and the way she is celebrated today, and how important her data still is in the field today.Claire is an Irish scientist working at Diamond Light Source, the UK's national synchrotron. She was fascinated by atoms and molecules as a teenager and has managed to make looking at them her career! She is currently investigating molecules of calcium carbonate that were made by 1,000 secondary school students as part of Project M. Claire believes that science should be accessible and enjoyable for all, at whatever level they choose to do explore it.

In the fifth episode of our 2018 NIJ R&D Season, Just Science speaks with Dr. Jamie Wieland and Dr. Christopher Mulligan of Illinois State University about assessing the impact of implementing portable mass spectrometers for on-site drug evidence processing. Listen along as Just Science explores cross-disciplinary research to determine the analytical, legal, and fiscal impacts of adopting drug screening protocols using portable mass spectrometers in the field. This season is funded by the National Institute of Justice’s Forensic Technology Center of Excellence.

Adebayo “Ade” Alonge is the Nigerian co-founder of RxAll, a platform which provides patients in the developing world with authenticated and verified medicines. Prior to this, Ade was a strategy consultant with the Boston Consulting Group, and before that, he spent eight years working a Sanofi, Roche, and BASF. In this absorbing, not-so-quick chat with Andile Masuku, Ade unpacks the state of play within Nigeria's pharmaceutical mass market, and explains how RxAll is enabling direct access to affordable, high-quality medicines while helping to reshape drug purchasing habits within markets rife with counterfeit product.

Shining a light on milk to reveal its secrets will allow 'point of cow diagnostics' about the quality of milk and the health of individual dairy cows.

Shining a light on milk to reveal its secrets will allow 'point of cow diagnostics' about the quality of milk and the health of individual dairy cows.

A discussion of the developments in nuclear physics that led to the discovery of fission.  These include Francis Aston's development of the mass spectrometer, George Gamow, Neils Bohr and Charles Weisacker and the development of the Liquid-Drop Model of the nucleus, the work of Otto Hahn at the Kaiser Wilhelm Institute in Berlin, Lise Meitner and Otto Frisch in discovering nuclear fission and both H. G. Wells and Leo Szilard's prophetic predictions of the development of atomic weapons.  

Nicholas Barbi, CEO of PulseTor. "A new portable X-Ray spectrometer designed for XRF analysis in cultural heritage applications".

How do we know what the stars are made of when we've never been to one? Dr Andrew Steele shows us how to make a spectrometer, a device used by scientists to analyse light, using a cereal box and a CD.

How do we know what the stars are made of when we've never been to one? Dr Andrew Steele shows us how to make a spectrometer, a device used by scientists to analyse light, using a cereal box and a CD.

This video is a tutorial on how to assemble and use a spectrometer using a CD diffraction grating and cellphone camera. Sample spectra of a white LED and red laser are also shown.

Tony Colaprete from NASA Ames Research Center discusses results from the LCROSS Solar Viewing NIR Spectrometer. This talk was part of the Short Course on Lunar Volatiles during the New Approaches to Lunar Ice Detection and Mapping workshop at the Keck Institute for Space Studies at Caltech on July 22, 2013.

Tony Colaprete from NASA Ames Research Center discusses results from the LCROSS Solar Viewing NIR Spectrometer. This talk was part of the Short Course on Lunar Volatiles during the New Approaches to Lunar Ice Detection and Mapping workshop at the Keck Institute for Space Studies at Caltech on July 22, 2013.

After traveling through the inner solar system for seven years, NASA's MESSENGER spacecraft reached Mercury in March 2011 and became the first ever mission to orbit this mysterious planet. Since then MESSENGER has been making measurements with its suite of scientific instruments including gamma-ray, neutron and x-ray spectrometers, magnetometer, laser altimeter, cameras and other instruments. Join Morgan Burks, a physicist at Lawrence Livermore National Laboratory, to explore the mysteries surrounding Mercury's formation and composition and the instruments that need to work at cryogenic temperatures in one of the hottest places in the solar system. Series: "Lawrence Livermore National Lab Science on Saturday" [Science] [Show ID: 24905]

After traveling through the inner solar system for seven years, NASA's MESSENGER spacecraft reached Mercury in March 2011 and became the first ever mission to orbit this mysterious planet. Since then MESSENGER has been making measurements with its suite of scientific instruments including gamma-ray, neutron and x-ray spectrometers, magnetometer, laser altimeter, cameras and other instruments. Join Morgan Burks, a physicist at Lawrence Livermore National Laboratory, to explore the mysteries surrounding Mercury's formation and composition and the instruments that need to work at cryogenic temperatures in one of the hottest places in the solar system. Series: "Lawrence Livermore National Lab Science on Saturday" [Science] [Show ID: 24905]

After traveling through the inner solar system for seven years, NASA's MESSENGER spacecraft reached Mercury in March 2011 and became the first ever mission to orbit this mysterious planet. Since then MESSENGER has been making measurements with its suite of scientific instruments including gamma-ray, neutron and x-ray spectrometers, magnetometer, laser altimeter, cameras and other instruments. Join Morgan Burks, a physicist at Lawrence Livermore National Laboratory, to explore the mysteries surrounding Mercury's formation and composition and the instruments that need to work at cryogenic temperatures in one of the hottest places in the solar system. Series: "Lawrence Livermore National Lab Science on Saturday" [Science] [Show ID: 24905]

After traveling through the inner solar system for seven years, NASA's MESSENGER spacecraft reached Mercury in March 2011 and became the first ever mission to orbit this mysterious planet. Since then MESSENGER has been making measurements with its suite of scientific instruments including gamma-ray, neutron and x-ray spectrometers, magnetometer, laser altimeter, cameras and other instruments. Join Morgan Burks, a physicist at Lawrence Livermore National Laboratory, to explore the mysteries surrounding Mercury's formation and composition and the instruments that need to work at cryogenic temperatures in one of the hottest places in the solar system. Series: "Lawrence Livermore National Lab Science on Saturday" [Science] [Show ID: 24905]

Halford discusses the NASA BARREL project and space weather. The Balloon Array for Radiation-belt Relativistic Electron Losses campaign will help study the Van Allen Radiation Belts and why they change over time by using balloons launched in Antarctica.TranscriptSpeaker 1: Spectrum's next. Speaker 2: Mm [inaudible]. Speaker 3: Welcome [00:00:30] to spectrum the science and technology show on k a l x Berkeley, a biweekly 30 minute program bringing you interviews featuring bay area scientists and technologists. Speaker 1: Good afternoon. I'm your host, Rick Karnofsky. Our guest today is Alexa Helford. Alexa is a postdoc at Dartmouth who studies based weather. She's involved with the balloon group there who recently finished their 2013 launch of the NASA barrel or [00:01:00] balloon array for radiation belt, relativistic electron losses campaign. 20 balloons. Went up in Antarctica in January and February. Next year there'll be doing it again. They're doing this to track where radiation goes when it leaves the radiation belts. Alex, I welcome to spectrum. Thank you. Can you talk to us a little bit about space weather? Speaker 3: Yeah, it is the coolest thing ever cause it's weather, but in space. What does that mean? So whenever you hear of like solar storms [00:01:30] or geomagnetic storms, which tend to make the news, that space weather, the sun always is spewing out junk at us. It's usually a combination of protons, electrons, and magnetic fields. Sometimes there's ions in there. Speaker 1: Well, but when that stuff Speaker 3: hits us, that space, whether it can sometimes create a geomagnetic storm, which is where we have our magnetic fields of the earth being completely rearranged and energy being transported normally into the inner magneto sphere where it can disrupt [00:02:00] things like satellites and eventually caused currently in our ionosphere, which can induce currents in the ground and that can cause problems for technologies even here on earth. Speaker 1: And how frequently do these problems crop up? It depends. So the Sun has an 11 year cycle where it, Speaker 3: it goes from having low activity, which we just came out of an incredibly quiet solar minimum just a few years ago and now we're starting to go into a region of higher activities. So we have a lot more [00:02:30] solar storms occurring. Speaker 1: It depends on the solar cycle. This one looks like it might be a little quieter than the last one, Speaker 3: but you can have multiple storms during the week. In the more northern or very southern regions of the world where you're near the polar caps, you are more effected bySpeaker 1: I sub storms, which can happen three times a day. People study space, weather, what do they hope to do? They hope to eventually it. Okay. Speaker 3: [00:03:00] Right now we are sometimes able to do now casting. So we can essentially tell you what the weather's like right now. And that's really good for us. We do, I mean can't just go outside and look. No, it's a little bit harder than that. No, I especially is putting together space weather packages and the van Allen probes are currently producing space weather data products as well. So we're getting a lot better at this. They usually give you at least a good, you know, [00:03:30] three or four days heads up as to if something's coming at us. They've gotten really, you know, pretty good given the type of data we have for even being able to predict if it's going to affect us or not. And what can we do with those predictions? So the radiation belts are where a lot of this, the damaging space weather effects occur. Speaker 3: They have highly relativistic electrons in them and these highly relativistic electrons can greatly affect ours [00:04:00] satellites. So what happens is any satellites sitting in the radiation belts actually will start gaining charge and we can get lightning strikes that actually occur across the [inaudible], the sides of the satellite, which in itself is quite damaging. Anytime you're hit by lightning is never really a good thing, but the really relativistic one's the killer electrons this week. Call them actually can bury themselves into the software and flip bits and so by flipping the bit they can send phantom [00:04:30] messages to the satellite and sometimes that message is to turn itself off or kill itself and not respond to ground control end. Essentially the satellite is dead floating in space. Satellite companies, when they find that there's going to be a solar storm that's going to hit us and possibly affect their spacecraft, they turn them off because if they turn them off then you know you're not going to get as much charging and you're not going to have as many problems. Speaker 3: What kinds of impacts do we see here on earth? So [00:05:00] back in 1989 there was a solar storm that actually induced currents in the power grid and blacked out. Most of the eastern seaboard of Canada and the North Eastern part of the u s and that was, that was quite a big problem where right now we've actually increased the connectivity of our power grids so that if the same storm were to happen about half the u s would be blacked out. Would there be actions that we could actually take if yes, so what you can do is you can actually turn off the grid or turn [00:05:30] off parts of the power grid so that you're not going to blow a transformer by having this huge amount of new current. In fact, one of the first things with space weather affecting our technology was way back with the telegraphs. They were able to run the telegraphs for hours without any energy because of the induced currents from the solar storms. Speaker 2: [inaudible]Speaker 4: are listening to k a l x Berkeley. [00:06:00] I'm talking with Alexa Helford about space weather. Speaker 3: We have stereo, which is one of the coolest missions ever, so it's two satellites. One is [inaudible], a head of earth around Earth orbit and the other one is falling behind [00:06:30] earth orbit and they're looking at the sun. So this is the first time we've ever had a three dimensional view of the sun and now they've gotten far enough around that. We're actually able to see what's going on behind the sun. So before we've always had to to kind of gas and use a Sonogram essentially. Yeah. To try to see what's on the other side of the sun. And now we have actual images of what's going on back there [00:07:00] and we're learning such amazing things from it. It's just the coolest thing ever. And besides, you get to wear 3d classes to view the pictures from it, which is always kind of cool. We're learning so much more about th what happens and, and how things are forming on the surface of the sun that it's really [inaudible] interesting time to kind of be a scientist and learning about [inaudible] this, you know, how space weather's happening. Speaker 3: Uh, besides that we have, you know, satellites in, in our own magnetosphere [00:07:30] that we can look at and we have ground-based magnetometers, which they're all really great with helping kind of understand the environment right now. What kinds of things do you have to measure and track and how do you track them in order to make predictions? That is really, that's an interesting question, but one of the cool things is, is us learning how to do all of this. Right now the ace satellite sits at the l one point, which is a stable orbit between the earth and the sun. We get magnetic [00:08:00] field particle data, so like densities and velocities, uh, from there, and we can use that to try to predict what it's coming at us. Unfortunately, what hits ace might not necessarily hit us, but it's our best predict. You're right now, it's coming to the end of its lifetime and we really need something up there, unfortunately, because we would want a space weather monitor up there, which [00:08:30] would help with science and research. Speaker 3: There's a fight going on as to who should be funding that and who wants to do that because it is, it is a large project, but it's something we need. Just like we need a tsunami warning systems. We need a space weather warning system. Can we talk about barrel a little bit? Yeah, so barrel is the campaign that I'm working on. Barrel is a, an array of that. We're going to be sending up in January of this year and January of [00:09:00] 2014 as well and possibly into February for both of those campaigns. Hopefully we'll be launching 20 balloons each year from two different stations in the antibiotics. So the British Halle Bay station and the South African Sinise station. And what we're going to do is these balloons are like what big weather balloons. They're going to be kind of drifting at 30 kilometers up in altitude and we'll be looking for x-rays. Speaker 3: [00:09:30] So when particles from space get perturbed during these geomagnetic storms, they can actually fall enough far enough down the field lines, these magnetic field lines that they'll hit the ionosphere in atmosphere where they can collide with different particles in neutral atoms and molecules and give off x-rays. And then we can measure those x-rays. So by backing out from that, that x-ray data, we can figure out what type of particles we're [00:10:00] being precipitated. So essentially we're looking at reins of highly relativistic particles and Artica we're looking in Antartica because if you remember your elementary school days when you played with bar magnets and, and iron fillings, you get, you know, if you have a bar magnet with the north and South Pole, you get these kind of curved arcs that go into and out of the northern and southern Poles. And the earth is just like that. So the earth is essentially a large [00:10:30] bar magnet and a, it has its dipole field that that kind of, you know, most of these field lines come in and out of the different poles. Speaker 3: And so when you're looking at these particles, they're going to be following those field lines. So they're just Tracy tracing out those lines that the iron fillings do with the bar magnet. And so these, these electrons and protons will come down the field lines and enter the atmosphere at the pole. So it's the best place to try to find stuff. And also there's not a whole [00:11:00] lot of things that the balloons can hit in the Antarctic, either from the two stations. The two stations give us a better range. And so by launching from both places, we'll be able to cover more land in Antarctica. And so at most we might have eight balloons up at any given time. And so we want to make sure that they're spaced as well as possible. You know, to be able to get the best coverage and having multiple loons up is going to give us an amazing opportunity that we [00:11:30] don't often have in space physics. You know by having multiple balloons, we're going to be able to take a look at how large some of these events are, how much ground they actually cover as well as how long they last. One of the things we can't answer is when you see these waves in space, how large are these waves? We know their wavelengths, but we don't know the region over which they occur. Speaker 2: [inaudible]Speaker 1: [00:12:00] this is spectrum on k a l x Berkeley. I'm Rick Karnofsky talking with Alexa Helford of the barrel project, a mission to study the van Allen radiation belts. Speaker 2: [inaudible]Speaker 1: [00:12:30] is barrel intentionally complementary to existing techniques? Speaker 3: Yeah, so in fact it is one of the first opportunity missions under the van Allen probes and so we're hoping to have conjugate measurements with them. So what that means is that we hope to essentially be on the same field minds as the satellites out in space. So while the satellites can measure the plasma out there and see these waves that are occurring in [00:13:00] space and see the different particles there, we're going to be able to then see how many of those particles actually made it down the field line. And it's one of the first missions with [inaudible] satellites and balloons that will really be able to do this. And, and hopefully because we're sending up 20 this year, hopefully we'll have lots of conjunctions. So that would be really great. And right now we're just Speaker 1: preparing for that. And do you have like a rough estimate of how high the satellites are versus how high the balloons are? Yes. Are the satellites, Speaker 3: they have [00:13:30] a pair of jeans. So their closest approach to the earth is, I believe around [inaudible], somewhere between three and 600 kilometers. So they're quite a bit higher. But when we have these conjunctions, these satellites are going to be at least four to six earth radii eye away from us. Speaker 1: So what kind of instrumentation is on these balloons? Speaker 3: So we are looking at, um, the magnetic fields. We have a gps transmitter there so that we can tell where [00:14:00] we are. That's kind of useful. And we have the [inaudible] Spectrometer, which is going to be looking at the x-rays and then we also have iridium phones essentially on there so we can actually get back our data quite quickly, which is very nice. It also means that we don't have to try to retrieve all 20 balloons. We've painted all of the payloads white and that's to actually help with the temperature control of all the instrumentation on board. But looking for it white Speaker 1: box [00:14:30] on a white continent turns out to be a very difficult thing. Right. And so these balloons go up, there's a small team over there and then you get all the data back at Dartmouth. Yes. What do you do with that? We are going to analyze it and have lots of fun working with all this data. Um, I'm really excited about it. We're also then going to be working Speaker 3: with the van Allen probes team and any other satellite mission that we can get in contact with that wants to look at our data. We're more than happy [00:15:00] to do that with. But having been an opportunity mission with the van Allen probe sets, the one we're really focusing on and really talking to and working with. So we're going to be looking at [inaudible] the different times when when we have uh, conjunctions and if there are any events. Now for this first mission, our conjunctions are going to be happening in the dawn sector. And so in the dawn sector, the waves that we're looking at are these micro bursts, which we [00:15:30] think are caused by course waves. Um, and this is going to be an exciting time cause it's one of the first times we're actually going to be able to look at this and, and, and be certain about it or relatively certain about it. And what's a course way, it's a course waves are these really fun little waves. They're caused by an electron, cyclotron instability. So it's all kind of generated by these electrons out in space. But if you listen to them, we can actually get way for them. So just like the radio waves you're hearing with us talking, [00:16:00] we get way forms of these, these waves in space and we can play them back through the radio and they sound like there. There sounds like a course of birds in the morning, which is why they're called course waves. Speaker 1: We have a recording of these course waves from the NASA van Allen probes. Speaker 2: [00:16:30] [inaudible] Speaker 4: the sound you just heard [00:17:00] was a chorus with an electromagnetic phenomenon caused by plasma waves in Earth's radiation belts. Hello, you're listening to spectrum on k a Alex Berkeley talking with Alexa Helford about space weather Speaker 2: [inaudible]Speaker 1: it's sort of like terrestrial weather [00:17:30] where so much can influence it. Oh, you rattled off a large list of different particles, all of which have different masses and, and um, would presumably hit us at different times, right? Yeah. Um, how, how do you possibly keep up with all that data? Speaker 3: Um, through statistics? That's what I love to do is data statistics and we're starting to get to a point where we have large enough databases to look at. And actually statistics [00:18:00] is, is, I mean, I know a lot of people hear the word statistics and they think, oh, boring, boring, boring. But it is just so cool. Um, because like you said, we're have so many different things going on and like tresha whether there's so many different factors that we don't necessarily know about, we think we understand what physics is up there. Um, but we know that we're missing some of it because our models don't exactly predict what's happening. So with a lot [00:18:30] of physics, when you're working in a lab, you can control everything. And so your theories can be directly tested because you can control every little bit to match the theory in space. Speaker 3: We can't control anything. It is our laboratory and we can't tell it what to do. We put satellites and balloons and ground-based magnetometers and, and all these different, uh, instruments out there and hope that something interesting happens. So do other planets also experienced space weather? [00:19:00] Yeah. Yeah, they do. In fact, it's, it's really kind of cool when you start looking at it. So mercury has its own little magnetosphere. It's much smaller than ours. So things happen on a much faster time scale. Right now there's a satellite out there called messenger, which is studying the space weather at mercury. And it's really neat to compare it to what we see on the earth because we can see things happening so much faster. So that's really neat. Venus has [00:19:30] some interesting stuff going on there. It doesn't have a magneto sphere, but we can, we can use that as another comparison cause it's a similar sized body to us. Speaker 3: And so it has interesting things on its own. Mars used to have a magnetosphere [inaudible] but Mars is really interesting because that's where we want to go and send people someday. And I really think we should because if anything, humans have always tried to explore and try to go out farther. And so Mars is our new new world, [00:20:00] but we have to be careful going there because it doesn't have the protection of a magnetosphere like we do. So in order to protect the astronauts, we need to have better space weather warning systems in play. And these are all things that people have been thinking much harder about than I ever had. But it's really an exciting thing to think about cause that that's solar wind, it doesn't stop when it hits us. It continues out there. Jupiter, Jupiter is a massive thing. Need a sphere. [00:20:30] It is so cool. Speaker 3: It even has a planet that has a magnetosphere. So there's a main Nita sphere inside of magnetosphere, but Jupiter's magnetosphere is dominated by io. I O sends out tons and tons of sulfur ions from volcanoes and so drives a lot of the main use for dynamics we see there. Saturn on the other hand doesn't have a volcanic moon, quite like Io. [00:21:00] It has other geysers which seem to develop its rings. But a lot of the, the space weather events we see in its magneto sphere actually come from the solar wind. But by the time the solar wind reaches Saturn, it is so diffuse. But we still see things like Aurora out there. We see Aurora on the, um, on the Jovian magnetosphere as well. Um, and that's just so cool. And then once you, you know, you get farther and farther out and each of the big gas giants has its own magnetosphere and they're all [00:21:30] unique in their own way and it just gives us so many different comparisons to our own planet so we can learn so much more by studying theirs as well, which is just kind of cool. Speaker 3: We've only been a field really since about 1957 when the first satellite, we're not, we mean people have been studying space weather for a lot longer than that. But you know, we weren't ever able to get measurements where stuff is happening before we had satellites. So we're right at the [00:22:00] beginning and it's something incredibly exciting time. Yeah. To be in the field cause we're just learning what it's like up there. There's so much we don't know. And every time we put up a new satellite we get back new data. Even if we thought that we'd just be seeing the same kind of thing, there's always something new happening. And so it's so incredibly exciting just to, to see what's out there. Well with that Alexa Alford, thanks for joining us. Thanks so much for having me Speaker 5: [inaudible]Speaker 6: [00:22:30] and now for some science news headlines. Here's an ana at Coolin and Renee Ralph Speaker 5: [inaudible],Speaker 6: professor in sleep expert, Matthew Walker explained in conversation with UC Berkeley new center that when we are young we have deep sleep that helps the brain store and retain new facts and information, but as we get older, the quality of our sleep [00:23:00] deteriorates and prevents those memories from being saved by the brain at night. In a recent study, UC Berkeley scientists discovered that there is a relationship between poor sleep, memory loss and brain deterioration. They found that poor sleep and old age affects memory loss. There are many stages of sleep, one of them being deep sleep, which is an important part of transporting short term memories to longterm memories. UC Berkeley researchers are now looking into therapeutic treatments for memory loss, such as electrical [00:23:30] stimulation to improve deep sleep and thus improve memory. You see, Berkeley researchers see this new discovery as an exciting opportunity to potentially help people remember more of their lives as they get older. Speaker 3: UC Berkeley have designed Speaker 6: a program to help decode ancient lost languages. Previously, human linguists have manually reconstructed languages by analyzing the relationships between the language and the patterns and sound change. The program takes modern [00:24:00] child languages, information about their word meaning and pronunciation and outputs, a rough approximation of the mother language. For example, if French and Spanish were input a language resembling Latin might emerge, the computer system we use together linkages across child languages to mathematically determine awards. First form. In a study published in the National Academy of Sciences Journal, the makers revealed that more than 85% of the system's reconstructions were identical to manual reconstructions [00:24:30] performed by linguist. Using this unique model, the system is essentially able to rewind the evolution of child languages all the way back to the original. The vast data crunching capabilities of the program have allowed scientists to begin seeing larger trends of spreading languages and banishing sounds well. Speaker 6: The computer system has extended the reach of computing in the field of linguistics. It's creators have stressed. They intend it to be used as a complimentary tool to human linguist, not as a replacement. A regular feature of spectrum [00:25:00] is a calendar of some of the science and technology related events happening in the bay area. Over the next two weeks, we'll hear once more from Anna and then Renee meet the animals up close at the Randall Museum home to over 100 animals that can not survive in the wild. Expect to see California wildlife such as rodents and fib. Ian's a great horned owl and even a tortoise every Saturday in March. Starting this Saturday, the ninth in San Francisco, doors open at 11:00 AM admission is free [00:25:30] in conjunction with San Francisco Sunday street program. The exploratorium. We'll have a day long road show featuring moving trucks with art, film, food, performances and activities. Speaker 6: The show will linger in three areas of the city, the mission Bayview and Embarcadero on its way to its nighttime finale at peer 15 this will take place in San Francisco this Sunday, March 10th from 11:00 AM to 10:00 PM for more information on performance times and locations, please visit [00:26:00] the exploratorium website which is exploratorium.edu stress and its effects on body and mind have always been biologically mysterious. This Monday, March 11th Dr Aaron Elica Nali will give her answers to some of those mysteries. Dr Canale is an assistant project scientist at the national primate research center in the Monday colloquium. She will speak about her research in the field of psychobiology. She will focus on the psychosocial effects of [00:26:30] early life stress. Dr [inaudible] has been studying relationships between biological and fostered offspring of rhesus monkey pairs and observing effects of exposure to early life stress on the relationships she has identified genes that cause physiological differences in the brain structure of these monkeys that suffered early stress. Speaker 6: She will also speak about the corresponding differences in the brains of human child abuse victims. The colloquium will be on March 11th from three to 4:30 PM in five [00:27:00] one-on-one Tolman hall on the UC Berkeley campus in case that's not enough science for one day. Also on March 11th Marvin l Cohen, professor of the Graduate School of physics at UC Berkeley will give a speech on condensed matter physics condensed matter physics is also known as goldilocks physics because its primary focuses are skills of energy, time and size that are somewhere in the middle. Consequently, this branch of physics has become one of the most interdisciplinary Professor Cohen will describe some of the fascinating [00:27:30] research involving semiconductors superconductors and nanoscience. He will also relay a few observations about Einstein and his seminar research in condensed matter physics. The free event is open to and aimed at all audiences and should provide an illuminating glimpse into a lesser known branch of physics. Speaker 6: It will be held on March 11th from five to 6:00 PM at the eye house on the corner of Bancroft and Piedmont. The march science at Cal lecture is titled Cloud spotting at Saturday [00:28:00] and titan learning about weather from a billion miles away. The talk will be given by a motto Adom Covex, a researcher in the astronomy department at UC Berkeley. He received his phd in physical chemistry in 2004 at cal studying the photochemical kinetics of hydrocarbon aerosols in planetary atmospheres. He will describe how measurements from telescopes on earth, the Cassini spacecraft that is still orbiting the Saturn system and the Huguenot probe that landed on the surface of Titan. [00:28:30] Saturn's largest moon all inform our knowledge of weather in the Saturn system. The lecture is scheduled for Saturday, March 16th at 11:00 AM and the genetics and plant biology building room 100 on the northwest corner of the UC Berkeley campus. Speaker 5: [inaudible]Speaker 4: the music you [00:29:00] heard during say show we spend the Stein and David from his album book and Acoustic Speaker 5: [inaudible].Speaker 4: It is released under a creative Commons license version 3.0 spectrum was recorded and edited by me, Rick Karnofsky and by Brad Swift. Thank you for listening to spectrum. You're happy to hear from listeners. If you have comments about the show, please send them to us via email. All right. Email address is spectrum [00:29:30] dot klx@yahoo.com join us in two weeks at this same time. Speaker 5: [inaudible]Speaker 4: [inaudible]. See acast.com/privacy for privacy and opt-out information.

Halford discusses the NASA BARREL project and space weather. The Balloon Array for Radiation-belt Relativistic Electron Losses campaign will help study the Van Allen Radiation Belts and why they change over time by using balloons launched in Antarctica.TranscriptSpeaker 1: Spectrum's next. Speaker 2: Mm [inaudible]. Speaker 3: Welcome [00:00:30] to spectrum the science and technology show on k a l x Berkeley, a biweekly 30 minute program bringing you interviews featuring bay area scientists and technologists. Speaker 1: Good afternoon. I'm your host, Rick Karnofsky. Our guest today is Alexa Helford. Alexa is a postdoc at Dartmouth who studies based weather. She's involved with the balloon group there who recently finished their 2013 launch of the NASA barrel or [00:01:00] balloon array for radiation belt, relativistic electron losses campaign. 20 balloons. Went up in Antarctica in January and February. Next year there'll be doing it again. They're doing this to track where radiation goes when it leaves the radiation belts. Alex, I welcome to spectrum. Thank you. Can you talk to us a little bit about space weather? Speaker 3: Yeah, it is the coolest thing ever cause it's weather, but in space. What does that mean? So whenever you hear of like solar storms [00:01:30] or geomagnetic storms, which tend to make the news, that space weather, the sun always is spewing out junk at us. It's usually a combination of protons, electrons, and magnetic fields. Sometimes there's ions in there. Speaker 1: Well, but when that stuff Speaker 3: hits us, that space, whether it can sometimes create a geomagnetic storm, which is where we have our magnetic fields of the earth being completely rearranged and energy being transported normally into the inner magneto sphere where it can disrupt [00:02:00] things like satellites and eventually caused currently in our ionosphere, which can induce currents in the ground and that can cause problems for technologies even here on earth. Speaker 1: And how frequently do these problems crop up? It depends. So the Sun has an 11 year cycle where it, Speaker 3: it goes from having low activity, which we just came out of an incredibly quiet solar minimum just a few years ago and now we're starting to go into a region of higher activities. So we have a lot more [00:02:30] solar storms occurring. Speaker 1: It depends on the solar cycle. This one looks like it might be a little quieter than the last one, Speaker 3: but you can have multiple storms during the week. In the more northern or very southern regions of the world where you're near the polar caps, you are more effected bySpeaker 1: I sub storms, which can happen three times a day. People study space, weather, what do they hope to do? They hope to eventually it. Okay. Speaker 3: [00:03:00] Right now we are sometimes able to do now casting. So we can essentially tell you what the weather's like right now. And that's really good for us. We do, I mean can't just go outside and look. No, it's a little bit harder than that. No, I especially is putting together space weather packages and the van Allen probes are currently producing space weather data products as well. So we're getting a lot better at this. They usually give you at least a good, you know, [00:03:30] three or four days heads up as to if something's coming at us. They've gotten really, you know, pretty good given the type of data we have for even being able to predict if it's going to affect us or not. And what can we do with those predictions? So the radiation belts are where a lot of this, the damaging space weather effects occur. Speaker 3: They have highly relativistic electrons in them and these highly relativistic electrons can greatly affect ours [00:04:00] satellites. So what happens is any satellites sitting in the radiation belts actually will start gaining charge and we can get lightning strikes that actually occur across the [inaudible], the sides of the satellite, which in itself is quite damaging. Anytime you're hit by lightning is never really a good thing, but the really relativistic one's the killer electrons this week. Call them actually can bury themselves into the software and flip bits and so by flipping the bit they can send phantom [00:04:30] messages to the satellite and sometimes that message is to turn itself off or kill itself and not respond to ground control end. Essentially the satellite is dead floating in space. Satellite companies, when they find that there's going to be a solar storm that's going to hit us and possibly affect their spacecraft, they turn them off because if they turn them off then you know you're not going to get as much charging and you're not going to have as many problems. Speaker 3: What kinds of impacts do we see here on earth? So [00:05:00] back in 1989 there was a solar storm that actually induced currents in the power grid and blacked out. Most of the eastern seaboard of Canada and the North Eastern part of the u s and that was, that was quite a big problem where right now we've actually increased the connectivity of our power grids so that if the same storm were to happen about half the u s would be blacked out. Would there be actions that we could actually take if yes, so what you can do is you can actually turn off the grid or turn [00:05:30] off parts of the power grid so that you're not going to blow a transformer by having this huge amount of new current. In fact, one of the first things with space weather affecting our technology was way back with the telegraphs. They were able to run the telegraphs for hours without any energy because of the induced currents from the solar storms. Speaker 2: [inaudible]Speaker 4: are listening to k a l x Berkeley. [00:06:00] I'm talking with Alexa Helford about space weather. Speaker 3: We have stereo, which is one of the coolest missions ever, so it's two satellites. One is [inaudible], a head of earth around Earth orbit and the other one is falling behind [00:06:30] earth orbit and they're looking at the sun. So this is the first time we've ever had a three dimensional view of the sun and now they've gotten far enough around that. We're actually able to see what's going on behind the sun. So before we've always had to to kind of gas and use a Sonogram essentially. Yeah. To try to see what's on the other side of the sun. And now we have actual images of what's going on back there [00:07:00] and we're learning such amazing things from it. It's just the coolest thing ever. And besides, you get to wear 3d classes to view the pictures from it, which is always kind of cool. We're learning so much more about th what happens and, and how things are forming on the surface of the sun that it's really [inaudible] interesting time to kind of be a scientist and learning about [inaudible] this, you know, how space weather's happening. Speaker 3: Uh, besides that we have, you know, satellites in, in our own magnetosphere [00:07:30] that we can look at and we have ground-based magnetometers, which they're all really great with helping kind of understand the environment right now. What kinds of things do you have to measure and track and how do you track them in order to make predictions? That is really, that's an interesting question, but one of the cool things is, is us learning how to do all of this. Right now the ace satellite sits at the l one point, which is a stable orbit between the earth and the sun. We get magnetic [00:08:00] field particle data, so like densities and velocities, uh, from there, and we can use that to try to predict what it's coming at us. Unfortunately, what hits ace might not necessarily hit us, but it's our best predict. You're right now, it's coming to the end of its lifetime and we really need something up there, unfortunately, because we would want a space weather monitor up there, which [00:08:30] would help with science and research. Speaker 3: There's a fight going on as to who should be funding that and who wants to do that because it is, it is a large project, but it's something we need. Just like we need a tsunami warning systems. We need a space weather warning system. Can we talk about barrel a little bit? Yeah, so barrel is the campaign that I'm working on. Barrel is a, an array of that. We're going to be sending up in January of this year and January of [00:09:00] 2014 as well and possibly into February for both of those campaigns. Hopefully we'll be launching 20 balloons each year from two different stations in the antibiotics. So the British Halle Bay station and the South African Sinise station. And what we're going to do is these balloons are like what big weather balloons. They're going to be kind of drifting at 30 kilometers up in altitude and we'll be looking for x-rays. Speaker 3: [00:09:30] So when particles from space get perturbed during these geomagnetic storms, they can actually fall enough far enough down the field lines, these magnetic field lines that they'll hit the ionosphere in atmosphere where they can collide with different particles in neutral atoms and molecules and give off x-rays. And then we can measure those x-rays. So by backing out from that, that x-ray data, we can figure out what type of particles we're [00:10:00] being precipitated. So essentially we're looking at reins of highly relativistic particles and Artica we're looking in Antartica because if you remember your elementary school days when you played with bar magnets and, and iron fillings, you get, you know, if you have a bar magnet with the north and South Pole, you get these kind of curved arcs that go into and out of the northern and southern Poles. And the earth is just like that. So the earth is essentially a large [00:10:30] bar magnet and a, it has its dipole field that that kind of, you know, most of these field lines come in and out of the different poles. Speaker 3: And so when you're looking at these particles, they're going to be following those field lines. So they're just Tracy tracing out those lines that the iron fillings do with the bar magnet. And so these, these electrons and protons will come down the field lines and enter the atmosphere at the pole. So it's the best place to try to find stuff. And also there's not a whole [00:11:00] lot of things that the balloons can hit in the Antarctic, either from the two stations. The two stations give us a better range. And so by launching from both places, we'll be able to cover more land in Antarctica. And so at most we might have eight balloons up at any given time. And so we want to make sure that they're spaced as well as possible. You know, to be able to get the best coverage and having multiple loons up is going to give us an amazing opportunity that we [00:11:30] don't often have in space physics. You know by having multiple balloons, we're going to be able to take a look at how large some of these events are, how much ground they actually cover as well as how long they last. One of the things we can't answer is when you see these waves in space, how large are these waves? We know their wavelengths, but we don't know the region over which they occur. Speaker 2: [inaudible]Speaker 1: [00:12:00] this is spectrum on k a l x Berkeley. I'm Rick Karnofsky talking with Alexa Helford of the barrel project, a mission to study the van Allen radiation belts. Speaker 2: [inaudible]Speaker 1: [00:12:30] is barrel intentionally complementary to existing techniques? Speaker 3: Yeah, so in fact it is one of the first opportunity missions under the van Allen probes and so we're hoping to have conjugate measurements with them. So what that means is that we hope to essentially be on the same field minds as the satellites out in space. So while the satellites can measure the plasma out there and see these waves that are occurring in [00:13:00] space and see the different particles there, we're going to be able to then see how many of those particles actually made it down the field line. And it's one of the first missions with [inaudible] satellites and balloons that will really be able to do this. And, and hopefully because we're sending up 20 this year, hopefully we'll have lots of conjunctions. So that would be really great. And right now we're just Speaker 1: preparing for that. And do you have like a rough estimate of how high the satellites are versus how high the balloons are? Yes. Are the satellites, Speaker 3: they have [00:13:30] a pair of jeans. So their closest approach to the earth is, I believe around [inaudible], somewhere between three and 600 kilometers. So they're quite a bit higher. But when we have these conjunctions, these satellites are going to be at least four to six earth radii eye away from us. Speaker 1: So what kind of instrumentation is on these balloons? Speaker 3: So we are looking at, um, the magnetic fields. We have a gps transmitter there so that we can tell where [00:14:00] we are. That's kind of useful. And we have the [inaudible] Spectrometer, which is going to be looking at the x-rays and then we also have iridium phones essentially on there so we can actually get back our data quite quickly, which is very nice. It also means that we don't have to try to retrieve all 20 balloons. We've painted all of the payloads white and that's to actually help with the temperature control of all the instrumentation on board. But looking for it white Speaker 1: box [00:14:30] on a white continent turns out to be a very difficult thing. Right. And so these balloons go up, there's a small team over there and then you get all the data back at Dartmouth. Yes. What do you do with that? We are going to analyze it and have lots of fun working with all this data. Um, I'm really excited about it. We're also then going to be working Speaker 3: with the van Allen probes team and any other satellite mission that we can get in contact with that wants to look at our data. We're more than happy [00:15:00] to do that with. But having been an opportunity mission with the van Allen probe sets, the one we're really focusing on and really talking to and working with. So we're going to be looking at [inaudible] the different times when when we have uh, conjunctions and if there are any events. Now for this first mission, our conjunctions are going to be happening in the dawn sector. And so in the dawn sector, the waves that we're looking at are these micro bursts, which we [00:15:30] think are caused by course waves. Um, and this is going to be an exciting time cause it's one of the first times we're actually going to be able to look at this and, and, and be certain about it or relatively certain about it. And what's a course way, it's a course waves are these really fun little waves. They're caused by an electron, cyclotron instability. So it's all kind of generated by these electrons out in space. But if you listen to them, we can actually get way for them. So just like the radio waves you're hearing with us talking, [00:16:00] we get way forms of these, these waves in space and we can play them back through the radio and they sound like there. There sounds like a course of birds in the morning, which is why they're called course waves. Speaker 1: We have a recording of these course waves from the NASA van Allen probes. Speaker 2: [00:16:30] [inaudible] Speaker 4: the sound you just heard [00:17:00] was a chorus with an electromagnetic phenomenon caused by plasma waves in Earth's radiation belts. Hello, you're listening to spectrum on k a Alex Berkeley talking with Alexa Helford about space weather Speaker 2: [inaudible]Speaker 1: it's sort of like terrestrial weather [00:17:30] where so much can influence it. Oh, you rattled off a large list of different particles, all of which have different masses and, and um, would presumably hit us at different times, right? Yeah. Um, how, how do you possibly keep up with all that data? Speaker 3: Um, through statistics? That's what I love to do is data statistics and we're starting to get to a point where we have large enough databases to look at. And actually statistics [00:18:00] is, is, I mean, I know a lot of people hear the word statistics and they think, oh, boring, boring, boring. But it is just so cool. Um, because like you said, we're have so many different things going on and like tresha whether there's so many different factors that we don't necessarily know about, we think we understand what physics is up there. Um, but we know that we're missing some of it because our models don't exactly predict what's happening. So with a lot [00:18:30] of physics, when you're working in a lab, you can control everything. And so your theories can be directly tested because you can control every little bit to match the theory in space. Speaker 3: We can't control anything. It is our laboratory and we can't tell it what to do. We put satellites and balloons and ground-based magnetometers and, and all these different, uh, instruments out there and hope that something interesting happens. So do other planets also experienced space weather? [00:19:00] Yeah. Yeah, they do. In fact, it's, it's really kind of cool when you start looking at it. So mercury has its own little magnetosphere. It's much smaller than ours. So things happen on a much faster time scale. Right now there's a satellite out there called messenger, which is studying the space weather at mercury. And it's really neat to compare it to what we see on the earth because we can see things happening so much faster. So that's really neat. Venus has [00:19:30] some interesting stuff going on there. It doesn't have a magneto sphere, but we can, we can use that as another comparison cause it's a similar sized body to us. Speaker 3: And so it has interesting things on its own. Mars used to have a magnetosphere [inaudible] but Mars is really interesting because that's where we want to go and send people someday. And I really think we should because if anything, humans have always tried to explore and try to go out farther. And so Mars is our new new world, [00:20:00] but we have to be careful going there because it doesn't have the protection of a magnetosphere like we do. So in order to protect the astronauts, we need to have better space weather warning systems in play. And these are all things that people have been thinking much harder about than I ever had. But it's really an exciting thing to think about cause that that's solar wind, it doesn't stop when it hits us. It continues out there. Jupiter, Jupiter is a massive thing. Need a sphere. [00:20:30] It is so cool. Speaker 3: It even has a planet that has a magnetosphere. So there's a main Nita sphere inside of magnetosphere, but Jupiter's magnetosphere is dominated by io. I O sends out tons and tons of sulfur ions from volcanoes and so drives a lot of the main use for dynamics we see there. Saturn on the other hand doesn't have a volcanic moon, quite like Io. [00:21:00] It has other geysers which seem to develop its rings. But a lot of the, the space weather events we see in its magneto sphere actually come from the solar wind. But by the time the solar wind reaches Saturn, it is so diffuse. But we still see things like Aurora out there. We see Aurora on the, um, on the Jovian magnetosphere as well. Um, and that's just so cool. And then once you, you know, you get farther and farther out and each of the big gas giants has its own magnetosphere and they're all [00:21:30] unique in their own way and it just gives us so many different comparisons to our own planet so we can learn so much more by studying theirs as well, which is just kind of cool. Speaker 3: We've only been a field really since about 1957 when the first satellite, we're not, we mean people have been studying space weather for a lot longer than that. But you know, we weren't ever able to get measurements where stuff is happening before we had satellites. So we're right at the [00:22:00] beginning and it's something incredibly exciting time. Yeah. To be in the field cause we're just learning what it's like up there. There's so much we don't know. And every time we put up a new satellite we get back new data. Even if we thought that we'd just be seeing the same kind of thing, there's always something new happening. And so it's so incredibly exciting just to, to see what's out there. Well with that Alexa Alford, thanks for joining us. Thanks so much for having me Speaker 5: [inaudible]Speaker 6: [00:22:30] and now for some science news headlines. Here's an ana at Coolin and Renee Ralph Speaker 5: [inaudible],Speaker 6: professor in sleep expert, Matthew Walker explained in conversation with UC Berkeley new center that when we are young we have deep sleep that helps the brain store and retain new facts and information, but as we get older, the quality of our sleep [00:23:00] deteriorates and prevents those memories from being saved by the brain at night. In a recent study, UC Berkeley scientists discovered that there is a relationship between poor sleep, memory loss and brain deterioration. They found that poor sleep and old age affects memory loss. There are many stages of sleep, one of them being deep sleep, which is an important part of transporting short term memories to longterm memories. UC Berkeley researchers are now looking into therapeutic treatments for memory loss, such as electrical [00:23:30] stimulation to improve deep sleep and thus improve memory. You see, Berkeley researchers see this new discovery as an exciting opportunity to potentially help people remember more of their lives as they get older. Speaker 3: UC Berkeley have designed Speaker 6: a program to help decode ancient lost languages. Previously, human linguists have manually reconstructed languages by analyzing the relationships between the language and the patterns and sound change. The program takes modern [00:24:00] child languages, information about their word meaning and pronunciation and outputs, a rough approximation of the mother language. For example, if French and Spanish were input a language resembling Latin might emerge, the computer system we use together linkages across child languages to mathematically determine awards. First form. In a study published in the National Academy of Sciences Journal, the makers revealed that more than 85% of the system's reconstructions were identical to manual reconstructions [00:24:30] performed by linguist. Using this unique model, the system is essentially able to rewind the evolution of child languages all the way back to the original. The vast data crunching capabilities of the program have allowed scientists to begin seeing larger trends of spreading languages and banishing sounds well. Speaker 6: The computer system has extended the reach of computing in the field of linguistics. It's creators have stressed. They intend it to be used as a complimentary tool to human linguist, not as a replacement. A regular feature of spectrum [00:25:00] is a calendar of some of the science and technology related events happening in the bay area. Over the next two weeks, we'll hear once more from Anna and then Renee meet the animals up close at the Randall Museum home to over 100 animals that can not survive in the wild. Expect to see California wildlife such as rodents and fib. Ian's a great horned owl and even a tortoise every Saturday in March. Starting this Saturday, the ninth in San Francisco, doors open at 11:00 AM admission is free [00:25:30] in conjunction with San Francisco Sunday street program. The exploratorium. We'll have a day long road show featuring moving trucks with art, film, food, performances and activities. Speaker 6: The show will linger in three areas of the city, the mission Bayview and Embarcadero on its way to its nighttime finale at peer 15 this will take place in San Francisco this Sunday, March 10th from 11:00 AM to 10:00 PM for more information on performance times and locations, please visit [00:26:00] the exploratorium website which is exploratorium.edu stress and its effects on body and mind have always been biologically mysterious. This Monday, March 11th Dr Aaron Elica Nali will give her answers to some of those mysteries. Dr Canale is an assistant project scientist at the national primate research center in the Monday colloquium. She will speak about her research in the field of psychobiology. She will focus on the psychosocial effects of [00:26:30] early life stress. Dr [inaudible] has been studying relationships between biological and fostered offspring of rhesus monkey pairs and observing effects of exposure to early life stress on the relationships she has identified genes that cause physiological differences in the brain structure of these monkeys that suffered early stress. Speaker 6: She will also speak about the corresponding differences in the brains of human child abuse victims. The colloquium will be on March 11th from three to 4:30 PM in five [00:27:00] one-on-one Tolman hall on the UC Berkeley campus in case that's not enough science for one day. Also on March 11th Marvin l Cohen, professor of the Graduate School of physics at UC Berkeley will give a speech on condensed matter physics condensed matter physics is also known as goldilocks physics because its primary focuses are skills of energy, time and size that are somewhere in the middle. Consequently, this branch of physics has become one of the most interdisciplinary Professor Cohen will describe some of the fascinating [00:27:30] research involving semiconductors superconductors and nanoscience. He will also relay a few observations about Einstein and his seminar research in condensed matter physics. The free event is open to and aimed at all audiences and should provide an illuminating glimpse into a lesser known branch of physics. Speaker 6: It will be held on March 11th from five to 6:00 PM at the eye house on the corner of Bancroft and Piedmont. The march science at Cal lecture is titled Cloud spotting at Saturday [00:28:00] and titan learning about weather from a billion miles away. The talk will be given by a motto Adom Covex, a researcher in the astronomy department at UC Berkeley. He received his phd in physical chemistry in 2004 at cal studying the photochemical kinetics of hydrocarbon aerosols in planetary atmospheres. He will describe how measurements from telescopes on earth, the Cassini spacecraft that is still orbiting the Saturn system and the Huguenot probe that landed on the surface of Titan. [00:28:30] Saturn's largest moon all inform our knowledge of weather in the Saturn system. The lecture is scheduled for Saturday, March 16th at 11:00 AM and the genetics and plant biology building room 100 on the northwest corner of the UC Berkeley campus. Speaker 5: [inaudible]Speaker 4: the music you [00:29:00] heard during say show we spend the Stein and David from his album book and Acoustic Speaker 5: [inaudible].Speaker 4: It is released under a creative Commons license version 3.0 spectrum was recorded and edited by me, Rick Karnofsky and by Brad Swift. Thank you for listening to spectrum. You're happy to hear from listeners. If you have comments about the show, please send them to us via email. All right. Email address is spectrum [00:29:30] dot klx@yahoo.com join us in two weeks at this same time. Speaker 5: [inaudible]Speaker 4: [inaudible]. Hosted on Acast. See acast.com/privacy for more information.

In this lab you will be exploring many aspects of optics. In class you learned about light polarization, Snell's law, critical angle, gratings, Fresnel equations and Brewster's angle. We will now be experimentally verifying all of these concepts.

We're on the hunt for dark matter, anti-matter, and why it matters

The SI-unit kilogram is scheduled to be re-defined within the next years. In the attempt to link it to a fundamental constant of nature – namely the Planck constant or the Avogadro constant – some discrepancies appeared. A direct determination of the molar Planck constant helps to trace this discrepancy. Such a determination can be done with the gamma-spectrometer Gams, that exists at the ILL. However, the instrument is not stable enough to provide the required accuracy of 2×10^(−8) (relative). To improve stability and accuracy, a complete new instrument was designed and built. For this purpose, the instrument core, an angle interferometer, had to be set up in vacuum. Drift-free fixation-methods and new designs for the optical elements, like corner-cube retro-reflectors, were developed. A new data acquisition system was elaborated, and also the mathematical theory to evaluate the acquired data. The new concepts for the instrument were completed, manufactured and assembled. First performance tests showed a quite convincing result in terms of stability. During the development of the new instrument, the old instrument Gams4 was optimized. The neutron binding energy of chlorine-36 was determined to be (8579797.4±1.8)eV. The relative uncertainty is 2.7 times smaller than the previous value. It is two times smaller than the uncertainty of any other comparable binding energy.

Four presenters of new medical technologies are today's featured guests. Benjamin Rhymer (a Registered Cardiovascular Invasive Specialist with the Cath Lab) describes how surgeries are performed inside the human heart without opening the chest using manipulation devices mounted on the end of long flexible catheters; he also discusses intravascular ultrasound cameras, and fluoroscopy. Laura Goldberg and Michelle Mekscer (of the Pathology Department at Aiken Regional Medical Centers Laboratory) describe how removed tissues are being examined microscopically in real time by specialists hundreds of miles away by sending live images from the microscope in the operating room to the specialist through the Internet. Doctor Chad Leverett (Associate Professor of Chemistry at USCA who is also a nanotechnology scientist working with the USC Nano Center in Columbia SC) describes his and the university's work in nanotechnology: including nanosensors, nanostructures and nanotechnology in medicine. He also explains the uses and technology of an infrared optical spectrometer which provides an instantaneous readout on a laptop computer of a sample's complete chemical and molecular composition. Hosted by Stephen Euin Cobb, this is the November 10, 2010 episode of The Future And You. [Running time: 32 minutes] These interviews were taped from the exhibition floor of the 2010  Business, Innovation and Technology Expo which was held on the campus of the University of South Carolina on July 17 2010.

Mon, 18 Jan 2010 12:00:00 +0100 https://edoc.ub.uni-muenchen.de/11059/ https://edoc.ub.uni-muenchen.de/11059/1/Laatiaoui_Mustapha.pdf Laatiaoui, Mustapha ddc:530, ddc:500, Fakultät für Physik

We look at the principles of operation of prism spectrometers and grating spectrometers and discuss operating characteristics (speed, resolving power, spectral transmission and free spectral range).

Transcript -- Astronomers compare events on other stars to helps us better understand our sun.

Astronomers compare events on other stars to helps us better understand our sun.

Transcript -- Astronomers compare events on other stars to helps us better understand our sun.

Astronomers compare events on other stars to helps us better understand our sun.

Tue, 17 Jun 2008 12:00:00 +0100 https://edoc.ub.uni-muenchen.de/8754/ https://edoc.ub.uni-muenchen.de/8754/1/Schweitzer_Mario.pdf Schweitzer, Mario

Airborne hyperspectral remote sensing enables not only spatial monitoring of vegetation cover, but also the derivation of individual plant constituents such as chlorophyll and nitrogen content. These are important parameters for optimised agricultural management on a field basis through the possibility of spatially differentiated fertilisation and for hydrological and vegetation yield modelling. The use of existing airborne imaging spectrometers is cost-intensive. Moreover, it is difficult to obtain these sensors for multitemporal applications. The imaging spectrometer AVIS (Airborne Visible/Near Infrared Imaging Spectrometer) was built at the Chair of Geography and Geographical Remote Sensing of the Ludwig Maximilians University Munich, Germany, to overcome these difficulties. AVIS is designed as a cost-effective tool for environmental monitoring using commonly available components. AVIS enables the deployment of a hyperspectral sensor for both scientific research and educational purposes. It is based on a direct sight spectrograph coupled to a standard B/W CCD camera. The signal received by the CCD is read out and sent via a frame grabber card to a personal computer, where the data is stored on the hard disc together with additional GPS data. The radiometric, spectral and geometric properties of AVIS resulting from the calibration procedure are summarised in Table 7-1. Table 7-1: AVIS characteristics Parameter Description Spectral range 553-999nm Spectral resolution 6nm Spectral sampling rate / resampling 2nm / 6nm Number of used bands 74 SNR 45dB (year 1999), 47dB (year 2000) Spatial resolution 300 pixels per image line Spatial sampling rate 390 pixels per image line FOV 1.19rad IFOV across track 3.1mrad IFOV along track 2.98mrad One aim of this thesis was to test the potential of AVIS for the purpose of environmental monitoring, especially of the chlorophyll and nitrogen status of plants. The land cover types under investigation were grassland, maize ( Zea mays L.) and winter wheat ( Triticum aestivum L.). Within this scope, a total of 21 AVIS flights were carried out during the vegetation periods of the years 1999 and 2000. The AVIS data were preprocessed before analysis, including dark current and flat field correction, resampling as well as atmospheric correction and reflectance calibration. The test area chosen for the validation of the AVIS data is located in the northern Bavarian foothills, 25km southwest of Munich, Germany (48° 6’ N, 11° 17’ E). It is situated between the Ammersee in the west and the Starnberger See in the east. The municipalities Gilching and Andechs define the northern and southern borders respectively. Within this area, three water protection areas were chosen as test sites. In these test sites, most of the farmers are under contract to the local agricultural office “ Amt für Landwirtschaft” resulting in detailed management data for each field. This data include useful information for the interpretation of ground and AVIS data. Two weather stations of the Bavarian network of agro-meteorological stations, namely No.72 (Gut Hüll) and No.80 (Rothenfeld), are located in the test area and provide information about precipitation, temperature and radiation. Ten and thirteen stands were selected as test fields in 1999 and 2000 respectively, including three fields each of maize and wheat in 1999 as well as three fields of maize and six fields of wheat in 2000. During both years, four meadows were investigated belonging to the same plant community ( Arrhenatherion elatioris). The meadows differ in the utilisation intensity (non-fertilised meadow with one cut, meadow with one cut, meadow with rotational grazing and meadow with four to five cuts). The ground truth campaigns included weekly measurements of plant parameters, such as height, dry and wet biomass, phenological stage, chlorophyll and nitrogen content, as well as a photographic documentation for each field. The chlorophyll and nitrogen measurements, which were derived from the sampling on ground, are available in contents per area [g/m²] and in contents per mass ([mg/g] for chlorophyll and [%DM] for nitrogen). The former can be used to evaluate the photosynthetic capacity or productivity of a canopy, which is an important input parameter for hydrological or vegetation models; the latter may be an indicator for plant physiological status or level of stress, which is a valuable source of information for optimising field management. The relationship between chlorophyll and nitrogen based on the ground measurements showed that a differentiation of the land cover types is necessary for significant correlation. When the plant species are investigated separately, the chlorophyll and nitrogen content per area are always highly correlated, especially for chlorophyll a and total chlorophyll content (r²≥0.8). For all investigated land cover types, the nitrogen and chlorophyll contents per mass are uncorrelated. For wheat, the results improve when the phenological state and the cultivar are considered (r²>0.67). For maize, distinct variations in the chlorophyll content per mass during the vegetation period reduced correlation with these parameters. The use of a fitted chlorophyll trend curve instead of the original measurements does not lead to a significant improvement of the results. For grassland, no significant correlation above r²=0.67 could be observed except for chlorophyll and nitrogen, both per area, where a decreasing strength of correlation could be monitored with increasing fertilisation level. These results lead to the conclusion that the chlorophyll and nitrogen contents per mass of the investigated land covers are decoupled when the compensation point for effective photosynthesis is exceeded. Beyond this limit the nitrogen in the plants is no longer incorporated into chlorophylls, but mainly into proteins, alkaloids and nucleic acids, whereas the proteins especially are used for internal storage of nitrogen. The derivation of the chlorophyll and nitrogen content of the plant leaves on a mean field basis was conducted using three hyperspectral spectral approaches, namely the hyperspectral NDVI (hNDVI), the Optimised Soil Adjusted Vegetation Index OSAVI as well as the relatively unknown Chlorophyll Absorption Integral CAI. The multispectral NDVITM was simulated as established reference. The results of the derivation of both chlorophyll and nitrogen content of plants with the investigated approaches depend strongly on a priori knowledge about the canopies monitored. In general, the use of contents per area rather than contents per mass has been found more suitable for the investigated remote sensing applications. A significant correlation between any index and the chlorophyll or nitrogen content for the whole sample size could not be derived. The optimal spectral approach for derivation is species-dependent, but also dependent on the cultivar. The chlorophyll and nitrogen level of the plants under observation as well as their temperature sensitivity mainly caused this dependence. The NDVITM, hNDVI and OSAVI became insensitive for high chlorophyll content above about 1g/m² (1.5mg/g) chlorophyll a and 0.2g/m² (0.4mg/g) chlorophyll b, respectively. A saturation of the indices was also found for nitrogen content above 2.5g/m². The saturation limit of nitrogen in percentage of dry matter could be rated at about 4%. The positive correlation between the indices and this parameter for wheat leads to insensitivity at values above this limit, while the negative correlation for maize results in saturation for values below 2.5%. The CAI is not affected by saturation as much as the other spectral approaches, leading to higher coefficients of determination, especially for contents per area. The CAI becomes insensitive at chlorophyll contents per area above 2g/m². The results lead to the assumption, that the flattening and narrowing of the chlorophyll absorption feature at 680nm most probably causes the saturation of the NDVITM, hNDVI and OSAVI. The ratios are directly affected by an increase in reflectance in the red wavelength region. The high correlations between the CAI and contents per area can be ascribed to the fact that the CAI is based on an integrated measurement over an area and therefore is less affected by an increase of reflectance in the red wavelengths. The CAI probably becomes insensitive at the point where the narrowing of the absorption feature leads to a shift of the red edge position towards the blue wavelength region. This saturation limit lies at approximately 2g chlorophyll per m². In contrast, the chlorophyll content per mass, which indicates the plant’s physiological status or level of stress, could be estimated more accurately using spectral indices such as hNDVI and OSAVI, especially for wheat. The low correlations derived for maize are caused by its higher temperature dependence, leading to daily variations in the chlorophyll content per mass. The chlorophyll and nitrogen contents of the grassland canopies could not be derived with the spectral approaches investigated. When the meadows were investigated separately, correlations could only be found between the CAI and the chlorophyll content per area for the most intensely utilised meadow (four to five cuts), which on the one side is characterised by the highest level of fertilisation, but on the other side is affected by the highest nutrient offtake. The low potential of the investigated indices can be mainly assigned to the fact that the chlorophyll and nitrogen values of the meadows mostly exceeded the saturation limits of the applied indices. The possibility of deriving chlorophyll and nitrogen accurately enough to map within field heterogeneities was discussed on the basis of a wheat field, which was analysed separately at three sampling points for chlorophyll and nitrogen content. The approaches found to be most suitable for the parameter estimation of wheat were applied. The CAI was used for the estimation of the chlorophyll content per area and mass as well as for the nitrogen content per area. The hNDVI was applied to estimate the canopy’s nitrogen content per mass. Both approaches were able to reproduce the chlorophyll contents of the different sampling points accurately enough to derive the differences between the measurement points when the saturation limits were not exceeded. Beyond these limits the index values decreased with increasing measurement values. The spatial pattern of the nutrient supply was discussed by comparing nitrogen pattern images, which were derived from CAI measurements acquired in 2000 with the yield measurement map of the same field. The phenological stage of stem elongation (EC 30) turned out to be most suitable for the derivation of the nitrogen pattern. On the one hand, the crop condition at these stages determine yield and on the other hand the nitrogen pattern images were able to map the inner field patterns of nitrogen supply. After anthesis the nitrogen images can map areas with different degrees of maturity. Therefore they can be used for the monitoring of maturity stages for the determination of the most favourable harvest date. As described here, AVIS is still in its early stages. It has the potential to become a costeffectiveAVIS2, which covers the spectral range of 400-900nm, has been in commercial use since 2001. tool for the monitoring of the environment. A modification of AVIS, namely

Wed, 27 Jun 2001 12:00:00 +0100 https://edoc.ub.uni-muenchen.de/351/ https://edoc.ub.uni-muenchen.de/351/1/Mengel_Sabine.pdf Mengel, Sabine ddc:530, d

Fri, 28 Jul 2000 12:00:00 +0100 https://edoc.ub.uni-muenchen.de/275/ https://edoc.ub.uni-muenchen.de/275/1/Deile_Mario.pdf Deile, Mario ddc:530, ddc:500, Fakul

A spectrometer system is presented for time-resolved probing in the midinfrared between 5 and 11 /tLmw ith a temporal resolution of better than 400 fs. Multichannel detection with HgCdTe detector arrays consisting of ten elements in combination with a high repetition rate permits one to record weak absorbance changes with an accuracy of 0.1 mOD.

A novel, simple, and inexpensive calibration scheme for a continuous-wave difference frequency spectrometer is presented, based on the stabilization of an open transfer cavity by locking onto the output of a polarization stabilized HeNe laser. High frequency, acoustic fluctuations of the transfer cavity length are compensated with a piezoelectric transducer mounted mirror, while long term drift in cavity length is controlled by thermal feedback. A single mode Ar+ laser, used with a single mode ring dye laser in the difference frequency generation of 2–4 µm light, is then locked onto a suitable fringe of this stable cavity, achieving a very small long term drift and furthermore reducing the free running Ar+ linewidth to about 1 MHz. The dye laser scan provides tunability in the difference frequency mixing process, and is calibrated by marker fringes with the same stable cavity. Due to the absolute stability of the marker cavity, precise frequency determination of near infrared molecular transitions is achieved via interpolation between these marker fringes. It is shown theoretically that the residual error of this scheme due to the dispersion of air in the transfer cavity is quite small, and experimentally that a frequency precision on the order of 1 MHz per hour is routinely obtained with respect to molecular transitions. Review of Scientific Instruments is copyrighted by The American Institute of Physics.