Podcast appearances and mentions of Star formation

What can gamma rays tell us about supernovae and galaxy formation? Neil deGrasse Tyson and co-host Chuck Nice sit down with astrophysicist Tim Paglione to explore high-energy cosmic phenomena, gamma rays, and the extreme events that create them.NOTE: StarTalk+ Patrons can listen to this entire episode commercial-free here:https://startalkmedia.com/show/the-extreme-universe-with-tim-paglione/Thanks to our Patrons Alexander Storts, Chris Henderson, Micheal Mayo, Jose Lotzin, Rebecca Noland, Scientific Panda, Sander Bergheim, Aubrey Loftus, John Leon, Jaquelin Butkovic, Jesse McIntyre, Kelly Sheffield, Kaseim カセイム, Bradley Westbrook, Chris Rassette, Aquahood, BA_MPH_JD_PhD-aspirant, Ravenwingfeather, Kaity Sturgell, Norma Bazan, Mickey Brumfield, lamar Gibson, Bong Bong, Andrew Hayes, Billy Madison, Bruce Muller, parker martindale, James Pope, Carrie Williams, Robert Lester, Mike Bundy, and My Pug is a Bug for supporting us this week. Subscribe to SiriusXM Podcasts+ on Apple Podcasts to listen to new episodes ad-free and a whole week early.

Mike and Chad invite astronomer Dr. Kathryn Devine to discuss the process of astronomy and how we can determine how stars form. Subscribe to the podcast to download the latest episode as soon as it is available.

We know that stars start with a cloud of gas and then turn into a glowing ball. But how exactly does this process happen? How do stars turn on? Astronomers have been using JWST to find out.

What does a black hole sound like? Neil deGrasse Tyson & Chuck Nice explore the sounds of the universe using JWST and Chandra X-Ray Observatory data with astrophysicist and data sonification expert Kimberly Arcand, Live at Guild Hall. NOTE: StarTalk+ Patrons can listen to this entire episode commercial-free.Thanks to our Patrons Deb, Linda Gibson, Dominic Hamken, JTsolept, Eric Sharakan, Rick Wallingford, Douglas Waltz, RT, Cristina, Lorraine Wright, Paul Deis, Diane Lapick, Dr. Staci Gruber, James Dorrough, Edward Bornman, GLENNA F MONTGOMERY, and David Martin for supporting us this week. Subscribe to SiriusXM Podcasts+ on Apple Podcasts to listen to new episodes ad-free and a whole week early.

This Q&A episode of Space Nuts is brought to you by Incogni. To check our special Space Nuts deal visit www.incogni.com/spacenutsSpace Nuts Q&A: Voyager's Journey, Star Formation, and Absolute Temperature Limits Join Andrew Dunkley and Professor Fred Watson in this engaging Q&A episode of Space Nuts, where they dive into intriguing listener questions about SpaceTime exploration, star formation, and the mysteries of temperature limits in the universe.Episode Highlights:Voyager's Future Path: Alan from Alberta asks about the future trajectory of Voyager 1 and 2. Discover what they might encounter in the distant future and the fascinating possibilities of their journey through interstellar SpaceTime.- Star Formation and Black Holes: Ron from New York brings up a complex topic about how supermassive black holes can quench star formation in galaxies. Fred Watson explains the mechanisms behind this phenomenon and the latest findings from the Webb Space Telescope.- Absolute Temperature Limits: Time to Take from Florida questions the upper limit of temperature in the universe. Explore the concept of absolute zero, the speed of light, and why there's no absolute maximum temperature.- Hypothetical Digestibility: Rennie poses a fun hypothetical about whether humans could digest plants and animals from another planet. Fred Watson and Andrew discuss the possibilities and potential risks.Don't forget to send us your questions for our Q&A episodes via our website... spacenuts.ioSupport Space Nuts and join us on this interstellar journey by visiting our website support page. Your contributions help us continue our mission to explore the wonders of the universe. Clear skies and boundless exploration await on Space Nuts, where we make the cosmos your backyard.Visit our websites:- www.spacenuts.io- www.bitesz.comBecome a supporter of this podcast: https://www.spreaker.com/podcast/space-nuts/support.

From July 3, 2024. Let's take a fast-paced journey thru all that's new in space and astronomy, including Mars Perseverance Rover fords an ancient river, black holes sometimes form like baby stars, and this week's tales from the launch pad. We also look in detail at how JWST images reveal star formation in never-before-seen details.   We've added a new way to donate to 365 Days of Astronomy to support editing, hosting, and production costs.  Just visit: https://www.patreon.com/365DaysOfAstronomy and donate as much as you can! Share the podcast with your friends and send the Patreon link to them too!  Every bit helps! Thank you! ------------------------------------ Do go visit http://www.redbubble.com/people/CosmoQuestX/shop for cool Astronomy Cast and CosmoQuest t-shirts, coffee mugs and other awesomeness! http://cosmoquest.org/Donate This show is made possible through your donations.  Thank you! (Haven't donated? It's not too late! Just click!) ------------------------------------ The 365 Days of Astronomy Podcast is produced by the Planetary Science Institute. http://www.psi.edu Visit us on the web at 365DaysOfAstronomy.org or email us at info@365DaysOfAstronomy.org.

Let's take a fast-paced journey thru all that's new in space and astronomy, including Mars Perseverance Rover fords an ancient river, black holes sometimes form like baby stars, and this week's tales from the launch pad. We also look in detail at how JWST images reveal star formation in never-before-seen details.

Researchers looked at lensed galaxy systems, searched for nearby analogs to those distant systems, and found that in general, the systems showed signs of bingeing star formation and then quiet lulls. Plus, using tree rings to track Arctic ice changes, and this week's What's Up.   We've added a new way to donate to 365 Days of Astronomy to support editing, hosting, and production costs.  Just visit: https://www.patreon.com/365DaysOfAstronomy and donate as much as you can! Share the podcast with your friends and send the Patreon link to them too!  Every bit helps! Thank you! ------------------------------------ Do go visit http://www.redbubble.com/people/CosmoQuestX/shop for cool Astronomy Cast and CosmoQuest t-shirts, coffee mugs and other awesomeness! http://cosmoquest.org/Donate This show is made possible through your donations.  Thank you! (Haven't donated? It's not too late! Just click!) ------------------------------------ The 365 Days of Astronomy Podcast is produced by the Planetary Science Institute. http://www.psi.edu Visit us on the web at 365DaysOfAstronomy.org or email us at info@365DaysOfAstronomy.org.

Hosted by Dr. Jacinta Delhaize & Dr. Daniel Cunnama. The IAU celebrates Women and Girls in Astronomy Month throughout February, from February 11th, 2022 in tandem with the United Nations' International Day of Women and Girls in Science, to International Women's Day on 8 March.   To celebrate this we speak with Dr. Elizabeth Naluminsa, a wonderful woman who is one of the first Ugandan women to obtain her PhD in Astronomy. Her dissertation topic was “Star Formation and Disk Stability in Nearby Galaxies”, which puts her at the forefront of galaxy evolution studies.   Liz is now working at the South African Astronomical Observatory with the Southern African Large Telescope ( SALT ) and she speaks with us about her work on SALT and SALT instrumentation.   We've added a new way to donate to 365 Days of Astronomy to support editing, hosting, and production costs.  Just visit: https://www.patreon.com/365DaysOfAstronomy and donate as much as you can! Share the podcast with your friends and send the Patreon link to them too!  Every bit helps! Thank you! ------------------------------------ Do go visit http://www.redbubble.com/people/CosmoQuestX/shop for cool Astronomy Cast and CosmoQuest t-shirts, coffee mugs and other awesomeness! http://cosmoquest.org/Donate This show is made possible through your donations.  Thank you! (Haven't donated? It's not too late! Just click!) ------------------------------------ The 365 Days of Astronomy Podcast is produced by the Planetary Science Institute. http://www.psi.edu Visit us on the web at 365DaysOfAstronomy.org or email us at info@365DaysOfAstronomy.org.

From June 25, 2009. Why was there a difference between the amount of matter and antimatter at the beginning of the Universe? Mathematics lets us travel faster than light speed, so why can't we? And are there stars forming around black holes?   - Why was there a difference between the amount of matter and antimatter at the beginning of the Universe? Do black holes have something to do with this? - Mathematically, we can have a velocity greater than the speed of lights lets us travel faster than light speed, so why can't we? - Can stars form in accretion disks around black holes? - How much precision is needed to keep space telescopes focused on one spot?  I have a hard enough time keeping my camera steady! - How can matter exist with antimatter? - What causes sunspots and do they influence Earth in any way? - How do we know what the speed of light is?  How can we measure something that fast and how did scientists figure that out? - Would life as we know it be able to survive around a Red Dwarf? - Could matter escape from the event horizon of two black holes colliding? - Why is it so bright in the center of the galaxy with a black hole there? - What is behind a black hole?   We've added a new way to donate to 365 Days of Astronomy to support editing, hosting, and production costs.  Just visit: https://www.patreon.com/365DaysOfAstronomy and donate as much as you can! Share the podcast with your friends and send the Patreon link to them too!  Every bit helps! Thank you! ------------------------------------ Do go visit http://www.redbubble.com/people/CosmoQuestX/shop for cool Astronomy Cast and CosmoQuest t-shirts, coffee mugs and other awesomeness! http://cosmoquest.org/Donate This show is made possible through your donations.  Thank you! (Haven't donated? It's not too late! Just click!) ------------------------------------ The 365 Days of Astronomy Podcast is produced by the Planetary Science Institute. http://www.psi.edu Visit us on the web at 365DaysOfAstronomy.org or email us at info@365DaysOfAstronomy.org.

Located at the edge of the Local Group, the Sagittarius Dwarf Irregular Galaxy has some of the stars with the fewest elements other than hydrogen or helium in the known universe.

Guest: Dr. Erin Macdonald Star Trek science advisor Dr. Erin Macdonald joins Mike to discuss the science behind Star Trek: Prodigy's first season, from protostars to red giants, damped sine waves to scientific ethics. Mike also asks Erin about her new children's book, Star Trek: My First Book of Space, and her cameo appearance in the Prodigy finale! Star Trek: My First Book of Space, by Dr. Erin Macdonald: https://www.penguinrandomhouse.com/books/710867/star-trek-my-first-book-of-space-by-erin-macdonald-phd-illustrated-by-jason-kayser/ Dr. Erin on Star Formation: https://www.youtube.com/watch?v=SWIVImXW3yY&ab_channel=ParamountPlus Homoploid hybrid speciation in the real world and in Star Trek: Prodigy by Prof. Mohamed Noor: https://www.youtube.com/watch?v=-PJbeySsqn0&ab_channel=BioTrekkieExplains%21 Follow us on Twitter! Strange New Worlds: https://twitter.com/scienceoftrek Mike: https://twitter.com/miquai Erin: https://twitter.com/drerinmac

Galaxy And Mass Assembly GAMA : The Dependence of Star Formation on Surface Brightness in Low Redshift Galaxies by S. Phillipps et al. on Wednesday 30 November The star formation rate in galaxies is well known to correlate with stellar mass (the `star-forming main sequence'). Here we extend this further to explore any additional dependence on galaxy surface brightness, a proxy for stellar mass surface density. We use a large sample of low redshift ($z leq 0.08$) galaxies from the GAMA survey which have both SED derived star formation rates and photometric bulge-disc decompositions, the latter providing measures of disc surface brightness and disc masses. Using two samples, one of galaxies fitted by a single component with S'{e}rsic index below 2 and one of the discs from two-component fits, we find that once the overall mass dependence of star formation rate is accounted for, there is no evidence in either sample for a further dependence on stellar surface density. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15998v1

The volumetric star formation law in nearby galaxies by C. Bacchini et al. on Wednesday 30 November Star formation laws are empirical relations between the cold gas (HI+H$_2$) content of a galaxy and its star formation rate (SFR), being crucial for any model of galaxy formation and evolution. A well known example of such laws is the Schmidt-Kennicutt law, which is based on the projected surface densities. However, it has been long unclear whether a more fundamental relation exists between the intrinsic volume densities. By assuming the vertical hydrostatic equilibrium, we infer radial profiles for the thickness of gaseous discs in a sample of 23 local galaxies, and use these measurements to convert the observed surface densities of the gas and the SFR into the de-projected volume densities. We find a tight correlation linking these quantities, that we call the volumetric star formation law. This relation and its properties have crucial implications for our understanding of the physics of star formation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16538v1

Morphology & Environment's Role on the Star Formation Rate -- Stellar Mass Relation in COSMOS from 0 < z < 3 5 by Kevin C. Cooke et al. on Wednesday 30 November We investigate the relationship between environment, morphology, and the star formation rate -- stellar mass relation derived from a sample of star-forming galaxies (commonly referred to as the `star formation main sequence') in the COSMOS field from 0 < z < 3.5. We constructed and fit the FUV--FIR SEDs of our stellar mass-selected sample of 111,537 galaxies with stellar and dust emission models using the public packages MAGPHYS and SED3FIT. From the best fit parameter estimates, we construct the star formation rate -- stellar mass relation as a function of redshift, local environment, NUVrJ color diagnostics, and morphology. We find that the shape of the main sequence derived from our color-color and sSFR-selected star forming galaxy population, including the turnover at high stellar mass, does not exhibit an environmental dependence at any redshift from 0 < z < 3.5. We investigate the role of morphology in the high mass end of the SFMS to determine whether bulge growth is driving the high mass turnover. We find that star-forming galaxies experience this turnover independent of bulge-to-total ratio, strengthening the case that the turnover is due to the disk component's specific star formation rate evolving with stellar mass rather than bulge growth. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16527v1

The volumetric star formation law in nearby galaxies by C. Bacchini et al. on Wednesday 30 November Star formation laws are empirical relations between the cold gas (HI+H$_2$) content of a galaxy and its star formation rate (SFR), being crucial for any model of galaxy formation and evolution. A well known example of such laws is the Schmidt-Kennicutt law, which is based on the projected surface densities. However, it has been long unclear whether a more fundamental relation exists between the intrinsic volume densities. By assuming the vertical hydrostatic equilibrium, we infer radial profiles for the thickness of gaseous discs in a sample of 23 local galaxies, and use these measurements to convert the observed surface densities of the gas and the SFR into the de-projected volume densities. We find a tight correlation linking these quantities, that we call the volumetric star formation law. This relation and its properties have crucial implications for our understanding of the physics of star formation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16538v1

PHANGS-JWST First Results: Duration of the early phase of massive star formation in NGC628 by Jaeyeon Kim et al. on Wednesday 30 November The earliest stages of star formation, when young stars are still deeply embedded in their natal clouds, represent a critical phase in the matter cycle between gas clouds and young stellar regions. Until now, the high-resolution infrared observations required for characterizing this heavily obscured phase (during which massive stars have formed, but optical emission is not detected) could only be obtained for a handful of the most nearby galaxies. One of the main hurdles has been the limited angular resolution of the Spitzer Space Telescope. With the revolutionary capabilities of the JWST, it is now possible to investigate the matter cycle during the earliest phases of star formation as a function of the galactic environment. In this Letter, we demonstrate this by measuring the duration of the embedded phase of star formation and the implied time over which molecular clouds remain inert in the galaxy NGC628 at a distance of 9.8Mpc, demonstrating that the cosmic volume where this measurement can be made has increased by a factor of $>100$ compared to Spitzer. We show that young massive stars remain embedded for $5.1_{-1.4}^{+2.7}$Myr ($2.3_{-1.4}^{+2.7}$Myr of which being heavily obscured), representing $sim20%$ of the total cloud lifetime. These values are in broad agreement with previous measurements in five nearby ($D < 3.5$Mpc) galaxies and constitute a proof of concept for the systematic characterization of the early phase of star formation across the nearby galaxy population with the PHANGS-JWST survey. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15698v1

Morphology & Environment's Role on the Star Formation Rate -- Stellar Mass Relation in COSMOS from 0 < z < 3 5 by Kevin C. Cooke et al. on Wednesday 30 November We investigate the relationship between environment, morphology, and the star formation rate -- stellar mass relation derived from a sample of star-forming galaxies (commonly referred to as the `star formation main sequence') in the COSMOS field from 0 < z < 3.5. We constructed and fit the FUV--FIR SEDs of our stellar mass-selected sample of 111,537 galaxies with stellar and dust emission models using the public packages MAGPHYS and SED3FIT. From the best fit parameter estimates, we construct the star formation rate -- stellar mass relation as a function of redshift, local environment, NUVrJ color diagnostics, and morphology. We find that the shape of the main sequence derived from our color-color and sSFR-selected star forming galaxy population, including the turnover at high stellar mass, does not exhibit an environmental dependence at any redshift from 0 < z < 3.5. We investigate the role of morphology in the high mass end of the SFMS to determine whether bulge growth is driving the high mass turnover. We find that star-forming galaxies experience this turnover independent of bulge-to-total ratio, strengthening the case that the turnover is due to the disk component's specific star formation rate evolving with stellar mass rather than bulge growth. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16527v1

On the ages of bright galaxies sim 500 Myr after the Big Bang: insights into star formation activity at z gtrsim 15 with JWST by Lily Whitler et al. on Wednesday 30 November With JWST, new opportunities to study the evolution of galaxies in the early Universe are emerging. Spitzer constraints on rest-optical properties of $zgtrsim7$ galaxies demonstrated the power of using galaxy stellar masses and star formation histories (SFHs) to indirectly infer the cosmic star formation history. However, only the brightest individual $zgtrsim8$ objects could be detected with Spitzer, making it difficult to robustly constrain activity at $zgtrsim10$. Here, we leverage the greatly improved rest-optical sensitivity of JWST at $zgtrsim8$ to constrain the ages of seven UV-bright ($M_{UV}lesssim-19.5$) galaxies selected to lie at $zsim8.5-11$, then investigate implications for $zgtrsim15$ star formation. We infer the properties of individual objects with two spectral energy distribution modelling codes, then infer a distribution of ages for bright $zsim8.5-11$ galaxies. We find a median age of $sim20$ Myr, younger than that inferred at $zsim7$ with a similar analysis, consistent with an evolution towards larger specific star formation rates at early times. The age distribution suggests that only $sim3$ percent of bright $zsim8.5-11$ galaxies would be similarly luminous at $zgtrsim15$, implying that the number density of bright galaxies declines by at least an order of magnitude between $zsim8.5-11$ and $zsim15$. This evolution is challenging to reconcile with some early JWST results suggesting the abundance of bright galaxies does not significantly decrease towards very early times, but we suggest this tension may be eased if young stellar populations form on top of older stellar components, or if bright $zsim15$ galaxies are observed during a burst of star formation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.01599v2

Statistical Study of the Star Formation Efficiency in Bars: Is Star Formation Suppressed in Gas-Rich Bars? by Fumiya Maeda et al. on Wednesday 30 November The dependence of star formation efficiency (SFE) on galactic structures, especially whether the SFE in the bar region is lower than those in the other regions, has recently been debated. We report the SFEs of 18 nearby gas-rich massive star-forming barred galaxies with a large apparent bar major axis ($geqq 75^{primeprime}$). We statistically measure the SFE by distinguishing the center, bar-end, and bar regions for the first time. The molecular gas surface density is derived from archival CO(1-0) and/or CO(2-1) data by assuming a constant CO-to-H$_2$ conversion factor ($alpha_{rm CO}$), and the star formation rate surface density is derived from a linear combination of far-ultraviolet and mid-infrared intensities. The angular resolution is $15^{primeprime}$, which corresponds to $0.3 - 1.8~rm kpc$. We find that the ratio of the SFE in the bar to that in the disk was systematically lower than unity (typically $0.6-0.8$), which means that the star formation in the bar is systematically suppressed. Our results are inconsistent with similar recent statistical studies that reported that SFE tends to be independent of galactic structures. This inconsistency can be attributed to the differences in the definition of the bar region, spatial resolution, $alpha_{rm CO}$, and sample galaxies. Furthermore, we find a negative correlation between SFE and velocity width of the CO spectrum, which is consistent with the idea that the large dynamical effects, such as strong shocks, large shear, and fast cloud-cloud collisions caused by the noncircular motion of the bar, result in a low SFE. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15681v1

Observational studies of high-mass star formation by Igor I. Zinchenko. on Wednesday 30 November We present a review of observational studies of high-mass star formation, based mainly on our own research. It includes surveys of high-mass star-forming regions in various molecular lines and in continuum, investigations of filamentary infrared dark clouds, which represent the earliest phases of massive star formation, detailed studies of individual high-mass star-forming regions, dense cores and disks harboring massive (proto)stars, and associated outflows. Chemistry in these regions is discussed, too. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15586v1

Galaxy And Mass Assembly GAMA : The Dependence of Star Formation on Surface Brightness in Low Redshift Galaxies by S. Phillipps et al. on Tuesday 29 November The star formation rate in galaxies is well known to correlate with stellar mass (the `star-forming main sequence'). Here we extend this further to explore any additional dependence on galaxy surface brightness, a proxy for stellar mass surface density. We use a large sample of low redshift ($z leq 0.08$) galaxies from the GAMA survey which have both SED derived star formation rates and photometric bulge-disc decompositions, the latter providing measures of disc surface brightness and disc masses. Using two samples, one of galaxies fitted by a single component with S'{e}rsic index below 2 and one of the discs from two-component fits, we find that once the overall mass dependence of star formation rate is accounted for, there is no evidence in either sample for a further dependence on stellar surface density. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15998v1

Disk dissipation, giant planet formation and star-formation-rate fluctuations in the past three-million-year history of Gould's Belt by Mingchao Liu et al. on Tuesday 29 November Although episodic star formation (SF) had been suggested for nearby SF regions, a panoramic view to the latest episodic SF history in the solar neighborhood is still missing. By uniformly constraining the slope $alpha$ of infrared spectral energy distributions (SEDs) of young stellar objects (YSOs) in the 13 largest Gould's Belt (GB) protoclusters surveyed by Spitzer Space Telescope, we have constructed a cluster-averaged histogram of $alpha$ representing YSO evolution lifetime as a function of the $alpha$ value. Complementary to the traditional SED classification scheme (0, I, F, II, III) that is based on different $alpha$ values, a staging scheme (A,B,C,D,E) of SED evolution is advised on the basis of the $alpha$ statistical features that can be better matched to the physical stages of disk dissipation and giant planet formation. This has also allowed us to unravel the fluctuations of star formation rate (SFR) in the past three-million-year (3 Myr) history of these GB protoclusters. Diverse evolutionary patterns such as single peak, double peaks and on-going acceleration of SFR are revealed. The SFR fluctuations are between $20%sim60%$ ($sim40%$ on average) and no dependence on the average SFR or the number of SFR episodes is found. However, spatially close protoclusters tend to share similar SFR fluctuation trends, indicating that the driving force of the fluctuations should be at size scales beyond the typical cluster sizes of several parsec. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.14637v1

Observational studies of high-mass star formation by Igor I. Zinchenko. on Tuesday 29 November We present a review of observational studies of high-mass star formation, based mainly on our own research. It includes surveys of high-mass star-forming regions in various molecular lines and in continuum, investigations of filamentary infrared dark clouds, which represent the earliest phases of massive star formation, detailed studies of individual high-mass star-forming regions, dense cores and disks harboring massive (proto)stars, and associated outflows. Chemistry in these regions is discussed, too. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15586v1

Statistical Study of the Star Formation Efficiency in Bars: Is Star Formation Suppressed in Gas-Rich Bars? by Fumiya Maeda et al. on Tuesday 29 November The dependence of star formation efficiency (SFE) on galactic structures, especially whether the SFE in the bar region is lower than those in the other regions, has recently been debated. We report the SFEs of 18 nearby gas-rich massive star-forming barred galaxies with a large apparent bar major axis ($geqq 75^{primeprime}$). We statistically measure the SFE by distinguishing the center, bar-end, and bar regions for the first time. The molecular gas surface density is derived from archival CO(1-0) and/or CO(2-1) data by assuming a constant CO-to-H$_2$ conversion factor ($alpha_{rm CO}$), and the star formation rate surface density is derived from a linear combination of far-ultraviolet and mid-infrared intensities. The angular resolution is $15^{primeprime}$, which corresponds to $0.3 - 1.8~rm kpc$. We find that the ratio of the SFE in the bar to that in the disk was systematically lower than unity (typically $0.6-0.8$), which means that the star formation in the bar is systematically suppressed. Our results are inconsistent with similar recent statistical studies that reported that SFE tends to be independent of galactic structures. This inconsistency can be attributed to the differences in the definition of the bar region, spatial resolution, $alpha_{rm CO}$, and sample galaxies. Furthermore, we find a negative correlation between SFE and velocity width of the CO spectrum, which is consistent with the idea that the large dynamical effects, such as strong shocks, large shear, and fast cloud-cloud collisions caused by the noncircular motion of the bar, result in a low SFE. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15681v1

Observational studies of high-mass star formation by Igor I. Zinchenko. on Tuesday 29 November We present a review of observational studies of high-mass star formation, based mainly on our own research. It includes surveys of high-mass star-forming regions in various molecular lines and in continuum, investigations of filamentary infrared dark clouds, which represent the earliest phases of massive star formation, detailed studies of individual high-mass star-forming regions, dense cores and disks harboring massive (proto)stars, and associated outflows. Chemistry in these regions is discussed, too. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15586v1

A Comprehensive Study on Galaxies at z~9-16 Found in the Early JWST Data: UV Luminosity Functions and Cosmic Star-Formation History at the Pre-Reionization Epoch by Yuichi Harikane et al. on Tuesday 29 November We conduct a comprehensive study on dropout galaxy candidates at $zsim9-16$ using the first 90 arcmin$^2$ JWST/NIRCam images taken by the early release observations (ERO) and early release science (ERS) programs. With the JWST simulation images, we find that a number of foreground interlopers are selected with a weak photo-$z$ determination ($Deltachi^2>4$). We thus carefully apply a secure photo-$z$ selection criterion ($Deltachi^2>9$) and conventional color criteria with confirmations of the ERO NIRSpec spectroscopic redshifts, and obtain a total of 23 dropout galaxies at $zsim9-16$, including two candidates at $z_mathrm{phot}=16.25_{-0.46}^{+0.24}$ and $16.41_{-0.55}^{+0.66}$. We perform thorough comparisons of dropout galaxies found in our work with recent JWST studies, and conclude that our galaxy sample is reliable enough for statistical analyses. We derive the UV luminosity functions at $zsim9-16$, and confirm that our UV luminosity functions at $zsim 9$ and $12$ agree with those determined by other HST and JWST studies. The cosmic star-formation rate density decreases from $zsim9$ to $12$, and perhaps to $16$, but the densities at $zsim12-16$ are higher than the constant star formation efficiency model. Interestingly, there are six bright galaxy candidates at $zsim10-16$ with $M_mathrm{UV}

PHANGS-JWST First Results: Duration of the early phase of massive star formation in NGC628 by Jaeyeon Kim et al. on Tuesday 29 November The earliest stages of star formation, when young stars are still deeply embedded in their natal clouds, represent a critical phase in the matter cycle between gas clouds and young stellar regions. Until now, the high-resolution infrared observations required for characterizing this heavily obscured phase (during which massive stars have formed, but optical emission is not detected) could only be obtained for a handful of the most nearby galaxies. One of the main hurdles has been the limited angular resolution of the Spitzer Space Telescope. With the revolutionary capabilities of the JWST, it is now possible to investigate the matter cycle during the earliest phases of star formation as a function of the galactic environment. In this Letter, we demonstrate this by measuring the duration of the embedded phase of star formation and the implied time over which molecular clouds remain inert in the galaxy NGC628 at a distance of 9.8Mpc, demonstrating that the cosmic volume where this measurement can be made has increased by a factor of $>100$ compared to Spitzer. We show that young massive stars remain embedded for $5.1_{-1.4}^{+2.7}$Myr ($2.3_{-1.4}^{+2.7}$Myr of which being heavily obscured), representing $sim20%$ of the total cloud lifetime. These values are in broad agreement with previous measurements in five nearby ($D < 3.5$Mpc) galaxies and constitute a proof of concept for the systematic characterization of the early phase of star formation across the nearby galaxy population with the PHANGS-JWST survey. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.15698v1

A global view on star formation: The GLOSTAR Galactic plane survey VII Supernova remnants in the Galactic longitude range 28^ circ

Disk dissipation, giant planet formation and star-formation-rate fluctuations in the past three-million-year history of Gould's Belt by Mingchao Liu et al. on Monday 28 November Although episodic star formation (SF) had been suggested for nearby SF regions, a panoramic view to the latest episodic SF history in the solar neighborhood is still missing. By uniformly constraining the slope $alpha$ of infrared spectral energy distributions (SEDs) of young stellar objects (YSOs) in the 13 largest Gould's Belt (GB) protoclusters surveyed by Spitzer Space Telescope, we have constructed a cluster-averaged histogram of $alpha$ representing YSO evolution lifetime as a function of the $alpha$ value. Complementary to the traditional SED classification scheme (0, I, F, II, III) that is based on different $alpha$ values, a staging scheme (A,B,C,D,E) of SED evolution is advised on the basis of the $alpha$ statistical features that can be better matched to the physical stages of disk dissipation and giant planet formation. This has also allowed us to unravel the fluctuations of star formation rate (SFR) in the past three-million-year (3 Myr) history of these GB protoclusters. Diverse evolutionary patterns such as single peak, double peaks and on-going acceleration of SFR are revealed. The SFR fluctuations are between $20%sim60%$ ($sim40%$ on average) and no dependence on the average SFR or the number of SFR episodes is found. However, spatially close protoclusters tend to share similar SFR fluctuation trends, indicating that the driving force of the fluctuations should be at size scales beyond the typical cluster sizes of several parsec. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.14637v1

Early Results From GLASS-JWST XVII: Building the First Galaxies -- Chapter 1 Star Formation Histories at 5

A Comprehensive Study on Galaxies at z~9-16 Found in the Early JWST Data: UV Luminosity Functions and Cosmic Star-Formation History at the Pre-Reionization Epoch by Yuichi Harikane et al. on Monday 28 November We conduct a comprehensive study on dropout galaxy candidates at $zsim9-16$ using the first 90 arcmin$^2$ JWST/NIRCam images taken by the early release observations (ERO) and early release science (ERS) programs. With the JWST simulation images, we find that a number of foreground interlopers are selected with a weak photo-$z$ determination ($Deltachi^2>4$). We thus carefully apply a secure photo-$z$ selection criterion ($Deltachi^2>9$) and conventional color criteria with confirmations of the ERO NIRSpec spectroscopic redshifts, and obtain a total of 23 dropout galaxies at $zsim9-16$, including two candidates at $z_mathrm{phot}=16.25_{-0.46}^{+0.24}$ and $16.41_{-0.55}^{+0.66}$. We perform thorough comparisons of dropout galaxies found in our work with recent JWST studies, and conclude that our galaxy sample is reliable enough for statistical analyses. We derive the UV luminosity functions at $zsim9-16$, and confirm that our UV luminosity functions at $zsim 9$ and $12$ agree with those determined by other HST and JWST studies. The cosmic star-formation rate density decreases from $zsim9$ to $12$, and perhaps to $16$, but the densities at $zsim12-16$ are higher than the constant star formation efficiency model. Interestingly, there are six bright galaxy candidates at $zsim10-16$ with $M_mathrm{UV}

A global view on star formation: The GLOSTAR Galactic plane survey VII Supernova remnants in the Galactic longitude range 28^ circ

Early Results From GLASS-JWST XVII: Building the First Galaxies -- Chapter 1 Star Formation Histories at 5

SpaceTime Series 25 Episode 127*How black holes control star formationNew observations using NASA's Webb Space Telescope are showing astronomers how black holes control star formation in galaxies.*Euclid completes thermal vacuum testingThe European Space Agency's new Euclid spacecraft has completed a key phase of its pre-flight thermal testing program as engineers and scientists prepare the probe for next year's launch to orbit.*Last Atlas V launch from CaliforniaSkywatchers have witnessed a bit of history with the last ever launch of an Atlas V rocket from the Californian coast.*More Chinese space junk pollutes low Earth orbitAnother Chinese rocket has exploded in orbit, The latest incident involved a Long March 6A rocket carrying the Yunhai 3 spy satellite into orbit from the Taiyuan Satellite Launch Center in Shanxi province.*The Science ReportDiscovery of a link between exposure to pollution and low birth weight in babies.A new breed of rice that could be more sustainable.Study finds that being young, male, religious, with a high income makes you more likely to gamble.Skeptics guide to avoiding hangoversListen to SpaceTime on your favorite podcast app with our universal listen link: https://spacetimewithstuartgary.com/listen For more SpaceTime and show links: https://linktr.ee/biteszHQ If you love this podcast, please get someone else to listen to. Thank you…To become a SpaceTime supporter and unlock commercial free editions of the show, gain early access and bonus content, please visit https://bitesz.supercast.com/ . Premium version now available via Spotify and Apple Podcasts.For more podcasts visit our HQ at https://biteszhq.com #space #astronomy #science #news #podcast #spacetime

The spatially resolved view of star formation in galaxy clusters by Bianca M. Poggianti et al. on Thursday 24 November Integral field spectroscopic studies of galaxies in dense environments, such as clusters and groups of galaxies, have provided new insights for understanding how star formation proceeds, and quenches. I present the spatially resolved view of the star formation activity and its link with the multiphase gas in cluster galaxies based on MUSE and multi-wavelength data of the GASP survey. I discuss the link among the different scales (i.e. the link between the spatially resolved and the global star formation rate-stellar mass relation), the spatially resolved signatures and the quenching histories of jellyfish (progenitors) and post-starburst (descendants) galaxies in clusters. Finally, I discuss the multi-wavelength view of star-forming clumps both in galaxy disks and in the tails of stripped gas. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12297v1

The spatially resolved view of star formation in galaxy clusters by Bianca M. Poggianti et al. on Wednesday 23 November Integral field spectroscopic studies of galaxies in dense environments, such as clusters and groups of galaxies, have provided new insights for understanding how star formation proceeds, and quenches. I present the spatially resolved view of the star formation activity and its link with the multiphase gas in cluster galaxies based on MUSE and multi-wavelength data of the GASP survey. I discuss the link among the different scales (i.e. the link between the spatially resolved and the global star formation rate-stellar mass relation), the spatially resolved signatures and the quenching histories of jellyfish (progenitors) and post-starburst (descendants) galaxies in clusters. Finally, I discuss the multi-wavelength view of star-forming clumps both in galaxy disks and in the tails of stripped gas. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12297v1

The dark side of galaxy stellar populations II: The dependence of star formation histories on halo mass and on the scatter of the main sequence by Laura Scholz-Diaz et al. on Wednesday 23 November Nearby galaxies are the end result of their cosmological evolution, which is predicted to be influenced by the growth of their host dark matter halos. This co-evolution potentially leaves signatures in present-day observed galaxy properties, which might be essential to further understand how the growth and properties of galaxies are connected to those of their host halos. In this work, we study the evolutionary histories of nearby galaxies both in terms of their host halos and the scatter of the star-forming main sequence by investigating their time-resolved stellar populations using absorption optical spectra drawn from the Sloan Digital Sky Survey. We find that galaxy star formation histories depend on the masses of their host halos, and hence they shape the evolution of the star-forming main sequence over cosmic time. Additionally, we also find that the scatter around the z=0 star-forming main sequence is not (entirely) stochastic, as galaxies with currently different star formation rates have experienced, on average, different star formation histories. Our findings suggest that dark matter halos might play a key role in modulating the evolution of star formation in galaxies, and thus of the main sequence, and further demonstrate that galaxies at different evolutionary stages contribute to the observed scatter of this relation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.11779v1

The spatially resolved view of star formation in galaxy clusters by Bianca M. Poggianti et al. on Wednesday 23 November Integral field spectroscopic studies of galaxies in dense environments, such as clusters and groups of galaxies, have provided new insights for understanding how star formation proceeds, and quenches. I present the spatially resolved view of the star formation activity and its link with the multiphase gas in cluster galaxies based on MUSE and multi-wavelength data of the GASP survey. I discuss the link among the different scales (i.e. the link between the spatially resolved and the global star formation rate-stellar mass relation), the spatially resolved signatures and the quenching histories of jellyfish (progenitors) and post-starburst (descendants) galaxies in clusters. Finally, I discuss the multi-wavelength view of star-forming clumps both in galaxy disks and in the tails of stripped gas. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12297v1

The dark side of galaxy stellar populations II: The dependence of star formation histories on halo mass and on the scatter of the main sequence by Laura Scholz-Diaz et al. on Tuesday 22 November Nearby galaxies are the end result of their cosmological evolution, which is predicted to be influenced by the growth of their host dark matter halos. This co-evolution potentially leaves signatures in present-day observed galaxy properties, which might be essential to further understand how the growth and properties of galaxies are connected to those of their host halos. In this work, we study the evolutionary histories of nearby galaxies both in terms of their host halos and the scatter of the star-forming main sequence by investigating their time-resolved stellar populations using absorption optical spectra drawn from the Sloan Digital Sky Survey. We find that galaxy star formation histories depend on the masses of their host halos, and hence they shape the evolution of the star-forming main sequence over cosmic time. Additionally, we also find that the scatter around the z=0 star-forming main sequence is not (entirely) stochastic, as galaxies with currently different star formation rates have experienced, on average, different star formation histories. Our findings suggest that dark matter halos might play a key role in modulating the evolution of star formation in galaxies, and thus of the main sequence, and further demonstrate that galaxies at different evolutionary stages contribute to the observed scatter of this relation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.11779v1

The Isaac Newton Telescope monitoring survey of Local Group dwarf galaxies--V The star formation history of Sagittarius dwarf irregular galaxy derived from long period variable stars by Tahere Parto et al. on Tuesday 22 November We conducted an optical monitoring survey of the Sagittarius dwarf irregular galaxy (SagDIG) during the period of June 2016 -- October 2017, using the 2.5-m Isaac Newton Telescope (INT) at La Palama. Our goal was to identify Long Period Variable stars (LPVs), namely asymptotic giant branch stars (AGBs) and red supergiant stars (RSGs), to obtain the Star Formation History (SFH) of isolated, metal-poor SagDIG. For our purpose, we used a method that relies on evaluating the relation between luminosity and the birth mass of these most evolved stars. We found $27$ LPV candidates within two half-light radii of SagDIG. $10$ LPV candidates were in common with previous studies, including one very dusty AGB (x-AGB). By adopting the metallicity $Z = 0.0002$ for older population and $Z=0.0004$ for younger ages, we estimated that the star formation rate changes from $0.0005pm0.0002$ M$_{odot}$yr$^{-1}$kpc$^{-2}$ ($13$ Gyr ago) to $0.0021 pm 0.0010$ M$_{odot}$yr$^{-1}$kpc$^{-2}$ ($0.06$ Gyr ago). Like many dwarf irregular galaxies, SagDIG has had continuous star formation activity across its lifetime, though with different rates, and experiences an enhancement of star formation since $z simeq 1$. We also evaluated the total stellar mass within two half-light radii of SagDIG for three choices of metallicities. For metallicity $Z = 0.0002$ and $Z=0.0004$ we estimated the stellar mass M$_*$ = ($5.4 pm 2.3$) $times$ $10^ 6$ and ($3.0 pm 1.3$) $times$ $10^ 6$ M$_{odot}$, respectively. Additionally, we determined a distance modulus $mu$ = $25.27pm0.05$ mag, using the tip of the red giant branch (TRGB). arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10695v1

The Isaac Newton Telescope monitoring survey of Local Group dwarf galaxies--V The star formation history of Sagittarius dwarf irregular galaxy derived from long period variable stars by Tahere Parto et al. on Monday 21 November We conducted an optical monitoring survey of the Sagittarius dwarf irregular galaxy (SagDIG) during the period of June 2016 -- October 2017, using the 2.5-m Isaac Newton Telescope (INT) at La Palama. Our goal was to identify Long Period Variable stars (LPVs), namely asymptotic giant branch stars (AGBs) and red supergiant stars (RSGs), to obtain the Star Formation History (SFH) of isolated, metal-poor SagDIG. For our purpose, we used a method that relies on evaluating the relation between luminosity and the birth mass of these most evolved stars. We found $27$ LPV candidates within two half-light radii of SagDIG. $10$ LPV candidates were in common with previous studies, including one very dusty AGB (x-AGB). By adopting the metallicity $Z = 0.0002$ for older population and $Z=0.0004$ for younger ages, we estimated that the star formation rate changes from $0.0005pm0.0002$ M$_{odot}$yr$^{-1}$kpc$^{-2}$ ($13$ Gyr ago) to $0.0021 pm 0.0010$ M$_{odot}$yr$^{-1}$kpc$^{-2}$ ($0.06$ Gyr ago). Like many dwarf irregular galaxies, SagDIG has had continuous star formation activity across its lifetime, though with different rates, and experiences an enhancement of star formation since $z simeq 1$. We also evaluated the total stellar mass within two half-light radii of SagDIG for three choices of metallicities. For metallicity $Z = 0.0002$ and $Z=0.0004$ we estimated the stellar mass M$_*$ = ($5.4 pm 2.3$) $times$ $10^ 6$ and ($3.0 pm 1.3$) $times$ $10^ 6$ M$_{odot}$, respectively. Additionally, we determined a distance modulus $mu$ = $25.27pm0.05$ mag, using the tip of the red giant branch (TRGB). arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10695v1

Sascha Zeegers is an astronomer researching interstellar dust, with Academia Sinica in Taiwan and scientists around the world. ICRT's Trevor Tortomasi chats with Sascha about her upcoming project with the James Webb Space Telescope, or JWST, and how these tiny dust particles throughout our galaxy play an important role in the birth of stars. Thanks for listening!

How American Racism Influenced Hitler https://www.newyorker.com/magazine/2018/04/30/how-american-racism-influenced-hitler The Impossibility of Translating Franz Kafka http://www.newyorker.com/magazine/1999/01/11/the-impossibility-of-being-kafka The Largest Alcohol Molecule Found in Space Yet May Be The Key to Star Formation https://www.sciencealert.com/this-is-the-largest-alcohol-molecule-we-ve-found-in-space-yet The Elemental Composition of the Human Body https://www.visualcapitalist.com/the-elemental-composition-of-the-human-body/ Life Helps Make Almost Half of Earth's Minerals https://www.quantamagazine.org/life-helps-make-almost-half-of-all-minerals-20220701/ A Logarithmic Map of the Entire Observable Universe https://www.visualcapitalist.com/cp/map-of-the-entire-known-universe/ ... Read more

Between her studies in star formation and her work with radio, optical, and infrared telescopes, Dr. Jennifer Wiseman has spent most of her life exploring the farthest reaches of the universe. Today we talked with Dr. Wiseman about what it's like to contemplate the cosmos for a living. How does her work inform her faith? What does astronomy teach us about humanity's place in the universe? And (we couldn't not ask): what's up with aliens?To learn more about Regent College and our upcoming courses, visit: www.regent-college.edu.

Hosts: Luke Pisani, Daniel Ogden, and Abby Williams Guest: Dr. Jeremy Bailin In this episode, Luke Pisani, Daniel Ogden, and Abby Williams talk with Dr. Jeremy Bailin, an associate professor in the Department of Physics and Astronomy in the College of Arts & Sciences. Dr. Bailin is particularly interested in galaxy formation and uses hydraulic computer simulation to study galaxies similar in size to the Milky Way. To check out more about Dr. Bailin, click here: https://physics.ua.edu/profiles/jeremy-bailin/.