POPULARITY
8 episodes with nircam
30 episodes with nircam
5 episodes with nircam
這張足清楚 ê 近紅外線相片是 James Webb 太空望遠鏡 翕--ê，中央有翕著 有環 ê 冰巨行星，海王星。這个暗淡 ê 遙遠世界是 離太陽上遠 ê 行星，差不多是地球到太陽距離 ê 30 倍遠。毋閣 tī 這个精彩 ê Webb 影像內底，這粒行星 暗甲親像是幽靈仝款，這是因為大氣層內底 ê 甲烷 kā 紅外線吸收了了。海王星表面大部份會吸收甲烷，伊頂懸 ê 懸雲，tī 這張相片內底嘛足明顯--ê。海王星上大粒 ê 衛星 海衛一 Triton 就 tī 這張 Webb 影像倒爿頂懸 ê 繞射光尖 遐。因為伊 ê 表面是堅凍 ê 窒素，所以伊比海王星反射太陽光閣較光。這張相片內底有 去 hŏng 揣著 海王星 14 粒衛星 ê 其中七粒，嘛包括海衛一 Triton。海王星 ê 環無遐爾光，伊就 tī 這張新翕--ê 太空行星肖像內底。這个複合環系統，是頭一擺翕甲遮爾清楚。頂擺翕著伊--ê，是 1989 年 8 月 ê 航海家 2 號太空船。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20240906/ 影像：NASA, ESA, CSA, STScI, NIRCam 音樂：高小糕 GaoXiaoGao 聲優：阿錕 翻譯：An-Li Tsai (NSYSU) 原文：https://apod.nasa.gov/apod/ap240906.html Powered by Firstory Hosting
Astronomy Daily - The Podcast: 13th September 2024Welcome to Astronomy Daily. I'm Anna, and you're tuning into your Daily dose of space and Astronomy news. We've got an action-packed episode for you today, filled with groundbreaking developments that are pushing the boundaries of human exploration and our understanding of the cosmos. Coming up, we'll dive into a historic milestone in private space exploration as SpaceX achieves the first-ever privately financed spacewalk. We'll also check in on Japan's ambitious plans for a second moon landing attempt and discuss the latest hurdles facing SpaceX's Starship program. But that's not all. We'll take you on a journey to the far reaches of our galaxy as the James Webb Space Telescope unveils stunning new observations of star formation in the extreme outer regions of the Milky Way. And finally, we'll explore NASA's efforts to establish a standardized lunar time, a crucial step for future moon missions and beyond. Stick around as we explore these fascinating stories and more on today's episode of Astronomy Daily.Highlights:- SpaceX's First Private Spacewalk: SpaceX has once again pushed the boundaries of commercial space exploration with a historic achievement. In a groundbreaking mission, billionaire Jared Isaacman and SpaceX crew trainer Sarah Gillis successfully conducted the first privately financed spacewalk in history. The spacewalk took place early Thursday morning, with Isaacman and Gillis taking turns floating just outside their Crew Dragon capsule at an altitude of 458 miles above Earth. They had an unobstructed view of our planet that left Isaacman in awe. This wasn't just a joyride in space, though. The primary goal of this 1 hour and 46 minutes spacewalk was to test SpaceX's new pressure suits. These new suits are a crucial development for SpaceX's ambitious plans to create low-cost, easy-to-manufacture spacesuits for future commercial astronauts who might one day fly to the moon or Mars aboard SpaceX's Super Heavy Starship rockets.- Japan's Second Moon Landing Attempt: Japanese space exploration company ispace is gearing up for another shot at the moon. Their second lunar landing mission is set to launch as early as December, just over a year and a half after their first attempt. The company's CEO, Takeshi Hakamada, announced that the Hakuto-R Mission 2 will be delivered to space aboard a SpaceX Falcon 9 rocket launching from Florida. After a journey of four to five months, the spacecraft will attempt its crucial lunar touchdown. Despite a setback in their first attempt, the company remains determined to achieve its goals.- SpaceX's Starship Program Delays: Their highly anticipated fifth test flight of its Starship rocket is facing unexpected delays. The Federal Aviation Administration (FAA) has announced that a final license determination for Starship Flight 5 is not expected before late November 2024. This comes as a setback for SpaceX, who had been gearing up for the launch since their successful fourth flight in June. The delay stems from SpaceX's decision to modify both the vehicle configuration and mission profile for Flight 5, triggering a more in-depth review process.- James Webb Space Telescope's New Discoveries: In a groundbreaking study, NASA's James Webb Space Telescope has turned its powerful gaze to the farthest reaches of our Milky Way, capturing stunning images of star-forming regions in what astronomers call the extreme outer galaxy. Using its NIRCam and MIRI instruments, the Webb telescope focused on two molecular clouds known as Deagle Clouds One and Two. These observations have revealed unprecedented details of star clusters undergoing intense bursts of star formation.- NASA's Standardized Lunar Time: NASA is taking on a task that might seem mundane at first glance but is actually crucial for future lunar missions: establishing a standardized lunar time. The space agency is spearheading efforts to create what's being called Coordinated Lunar Time (LTC). This initiative comes in response to a White House policy directive issued in April, recognizing the need for a unified timekeeping system on the moon. This lunar time standard isn't just about the moon, though. NASA sees it as a scalable solution that could be applied to future Mars missions and exploration of other celestial bodies in our solar system.For more space news, be sure to visit our website at astronomydaily.io. There you can sign up for our free Daily newsletter, catch up on all the latest space and Astronomy news with our constantly updating news feed, and listen to all our back episodes.Don't forget to follow us on social media. Just search for #AstroDailyPod on Facebook, X, YouTubeMusic, and TikTok to stay connected with our community and never miss an update.Thank you for tuning in, and remember to keep your eyes on the skies. Until next time, keep looking up.Sponsor Links:NordVPNNordPassMalwarebytesProton MailBecome a supporter of this Podcast for commercial-free editions: https://www.spreaker.com/podcast/astronomy-daily-the-podcast--5648921/support
這張 巨蛇座星雲 是 James Webb 太空望遠鏡 翕--ê 特寫相片，有翕著 ùi 新誕生恆星 噴出來 ê 物質流。能量足強 ê 原恆星噴流 是 雙極--ê，是 噴 tùi 相反方向 ê 雙噴流。In ê 噴射方向 kah 吸積盤 是 互相垂直--ê。吸積盤是 踅 恆星紅嬰仔stellar infants 咧行 ê 結構。恆星紅嬰仔 是 星雲 重力崩塌，開始自轉 ê 階段。這張 NIRcam 影像內底 ê 紅光，是水素分子 kah 一酸化炭素分子 ê 輻射。這是噴射流 kah 邊仔 ê 氣體塗粉相挵 產生--ê。這是頭一擺翕著 遮爾清楚 ê 影像。Tī 巨蛇座星雲 內底 翕--著 ê 噴流，攏噴 tùi 仝一个方向去。這个結果 kah 科學家 ê 料想結果 相 siâng。毋過一直到今，Webb 影像才有法度 tùi 這款活跳 ê 少年恆星形成區 進行 較詳細 ê 探索。較光 ê 前景星，會出現 Webb 影像特別有 ê 繞射光針。照 巨蛇座星雲 估計 ê 距離 1300 光年來算，這張宇宙特寫差不多有 1 光年闊。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20240627/ 影像：NASA, ESA, CSA, STScI, Klaus Pontoppidan (NASA-JPL), Joel Green (STScI) 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NSYSU) 原文：https://apod.nasa.gov/apod/ap240627.html Powered by Firstory Hosting
這幅深空視野拼鬥圖 leh 展示一个 hŏng 足讚嘆 ê 景色，這是 James Webb 太空望遠鏡 ê NIRCam 紀錄 loài ê 星系團 Abell 2744。Abell 2744 嘛叫做 Pandora 星系團，伊敢若是 3 个無仝 ê 大質量星系團合併 ê 結果。伊就 tī 玉夫座方向 35 億光年遠 ê 所在。這个大型星系團 因為 內底攏是烏暗物質，所以伊就 kā 時空扭曲去，這个 重力透鏡 效應嘛 影響著 閣較遠方 ê 天體。比 Pandora 星系團閣較紅 ê 天體，有足濟攏是受著透鏡效應 ê 影響，in 大部份攏是早期宇宙 ê 遙遠星系。受著透鏡效應扭曲 ê 影響，in ê 影像 去予搝長、拗彎，變做弧形。是講影像內底這寡 特別 ê 繞射光針，是銀河內 ê 前景星。照目前估計 ê Pandora 星系團 距離來看，這个宇宙盒仔差不多有 600 萬 光年大。毋過免驚！你閣會當看 這支 2 分鐘 ê 影片，來探索這个迷人 ê 天區。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20240608/ 影像來源：NASA, ESA, CSA, Ivo Labbe (Swinburne), Rachel Bezanson (University of Pittsburgh) 資料處理：Alyssa Pagan (STScI) 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NSYSU) 原文：https://apod.nasa.gov/apod/ap240608.html Powered by Firstory Hosting
A team of astronomers has used NASA's James Webb Space Telescope to survey the starburst galaxy Messier 82 (M82). Located 12 million light-years away in the constellation Ursa Major, this galaxy is relatively compact in size but hosts a frenzy of star formation activity. For comparison, M82 is sprouting new stars 10 times faster than the Milky Way galaxy.Led by Alberto Bolatto at the University of Maryland, College Park, the team directed Webb's NIRCam (Near-Infrared Camera) instrument toward the starburst galaxy's center, attaining a closer look at the physical conditions that foster the formation of new stars.“M82 has garnered a variety of observations over the years because it can be considered as the prototypical starburst galaxy,” said Bolatto, lead author of the study. “Both NASA's Spitzer and Hubble space telescopes have observed this target. With Webb's size and resolution, we can look at this star-forming galaxy and see all of this beautiful, new detail.”Star formation continues to maintain a sense of mystery because it is shrouded by curtains of dust and gas, creating an obstacle in observing this process. Fortunately, Webb's ability to peer in the infrared is an asset in navigating these murky conditions. Additionally, these NIRCam images of the very center of the starburst were obtained using an instrument mode that prevented the very bright source from overwhelming the detector.While dark brown tendrils of heavy dust are threaded throughout M82's glowing white core even in this infrared view, Webb's NIRCam has revealed a level of detail that has historically been obscured. Looking closer toward the center, small specks depicted in green denote concentrated areas of iron, most of which are supernova remnants. Small patches that appear red signify regions where molecular hydrogen is being lit up by a nearby young star's radiation.“This image shows the power of Webb,” said Rebecca Levy, second author of the study at the University of Arizona, Tucson. “Every single white dot in this image is either a star or a star cluster. We can start to distinguish all of these tiny point sources, which enables us to acquire an accurate count of all the star clusters in this galaxy.”Looking at M82 in slightly longer infrared wavelengths, clumpy tendrils represented in red can be seen extending above and below the galaxy's plane. These gaseous streamers are a galactic wind rushing out from the core of the starburst.One area of focus for this research team was understanding how this galactic wind, which is caused by the rapid rate of star formation and subsequent supernovae, is being launched and influencing its surrounding environment. By resolving a central section of M82, scientists could examine where the wind originates, and gain insight on how hot and cold components interact within the wind.Webb's NIRCam instrument was well-suited to trace the structure of the galactic wind via emission from sooty chemical molecules known as polycyclic aromatic hydrocarbons (PAHs). PAHs can be considered as very small dust grains that survive in cooler temperatures but are destroyed in hot conditions.Much to the team's surprise, Webb's view of the PAH emission highlights the galactic wind's fine structure – an aspect previously unknown. Depicted as red filaments, the emission extends away from the central region where the heart of star formation is located. Another unanticipated find was the similar structure between the PAH emission and that of hot, ionized gas.“It was unexpected to see the PAH emission resemble ionized gas,” said Bolatto. “PAHs are not supposed to live very long when exposed to such a strong radiation field, so perhaps they are being replenished all the time. It challenges our theories and shows us that further investigation is required.”Webb's observations of M82 in near-infrared light spur further questions about star formation, some of which the team hopes to answer with additional data gathered with Webb, including that of another starburst galaxy. Two other papers from this team characterizing the stellar clusters and correlations among wind components of M82 are almost finalized.In the near future, the team will have spectroscopic observations of M82 from Webb ready for their analysis, as well as complementary large-scale images of the galaxy and wind. Spectral data will help astronomers determine accurate ages for the star clusters and provide a sense of timing for how long each phase of star formation lasts in a starburst galaxy environment. On a broader scale, inspecting the activity in galaxies like M82 can deepen astronomers' understanding of the early universe.“Webb's observation of M82, a target closer to us, is a reminder that the telescope excels at studying galaxies at all distances,” said Bolatto. “In addition to looking at young, high-redshift galaxies, we can look at targets closer to home to gather insight into the processes that are happening here – events that also occurred in the early universe.”
The craft's NIRCam filters captured the planet, including its rings, in unprecedented detail.
毛蟹星雲 是 彼个有名 ê Charles Messier 星表 ê 頭一粒天體。伊 ê 編號是 M1，毋是彗星。天文學家 tī 1054 年 ê 時陣 to̍h 有發現伊 矣。實際上，咱這馬已經知影 毛蟹星雲 其實是一个 超新星殘骸，是大質量恆星死亡爆炸了後 ê 雲屑仔。這張清楚 ê 影像是 ùi James Webb 太空望遠鏡 ê 近紅外線相機 NIRCam kah 中紅外線儀器 MIRI 做伙提著 ê 觀測資料，是 tī 紅外線波段探索 猶咧脹大 ê 星際雲屑仔 發--出 ê 奇怪光線。對現代天文學家來講，其中上特別 ê 天體是 毛蟹星雲脈動星，to̍h 是相片中央上光彼粒，這是一粒一秒鐘踅 30 擺 ê 中子星。這粒恆星核心崩塌 ê 殘骸 to̍h kah 宇宙發電機 仝款，伊是毛蟹星雲 ê 動力來源，予伊 tī 電磁波頻譜產生發射線。毛蟹星雲差不多有 12 光年闊，伊 tī 金牛座 內底，離咱干焦 6500 光年遠爾爾。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20231109/ 影像：NASA, ESA, CSA, STScI; Tea Temim (Princeton University) 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NSYSU) 原文：https://apod.nasa.gov/apod/ap231109.html Powered by Firstory Hosting
暗星雲 L1527 內底 ê 原恆星 干焦 10 萬歲爾爾，伊這馬猶藏 tī 飼伊大漢 ê 氣體塗粉雲內底。這張是 James Webb 太空望遠鏡 ê NIRCam 翕 ê 紅外線相片。Tī 星雲頷頸有一條暗帶，彼其實是踅 tī 少年恆星 外口 厚 tut-tut ê 原恆星盤。Ùi Webb 望遠鏡 ê 紅外線影像看來，原恆星 是藏 tī 原恆星盤內底。這塊 原恆星盤 是側向--ê，比咱 ê 太陽系較大淡薄仔。伊 ê 物質，落尾會提去做原恆星。是講這張影像內底有濟濟星雲 ê 細節。這个沙漏形星雲，是去予原恆星發出 ê 紅外線 kā 照予光--ê。這是恆星形成過程中，去予 擲出來 ê 物質 kā 週邊媒介物掃出去 ê 結果。原恆星得著夠額 ê 質量了後，就會開始轉大人，產生重力崩塌，tī 核心開始進行核融合反應。暗星雲 L1527 內底 ê 原恆星 離 金牛座內底 ê 恆星形成區 有 460 光年遠。伊可能 kah 咱太陽系 tī 紅嬰仔時期有相仝。這張 Webb ê NIRCam 影像 差不多有 0.3 光年闊。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20221118/ 影像來源：科學：NASA, ESA, CSA, STScI, NIRCam 資料處理：Joseph DePasquale (STScI), Anton M. Koekemoer (STScI), Alyssa Pagan (STScI) 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NCU) 原文：https://apod.nasa.gov/apod/ap221118.html Powered by Firstory Hosting
During our November 16th show, Carolyn Collins Petersen introduced us to the hourglass/butterfly of L1527, an image captured by JWST using its onboard NIRCam. (You can read the original story here. This week we are joined by Dr. Karl Stapelfeldt, Chief Scientist for NASA's Exoplanet Exploration Program at JPL who will help us understand the science behind this amazing structure. Karl earned a B.S.E. in Aerospace Engineering and Engineering Physics at Princeton University, and a Ph.D. in Astrophysics at Caltech. His career at NASA includes positions at both the Jet Propulsion Laboratory and most recently at the Goddard Space Flight Center, where he has served as the Chief of Goddard's Exoplanets and Stellar Astrophysics Laboratory since 2011. Karl's NASA science contributions include project science roles for the Hubble and Spitzer Space Telescopes and science observations using the Herschel Space Observatory. He served as chair of the Exoplanet-Coronagraph Probe-Scale Science and Technology Definition Team, and as a member of the Astrophysics Subcommittee of the NASA Advisory Council. **************************************** The Weekly Space Hangout is a production of CosmoQuest. Want to support CosmoQuest? Here are some specific ways you can help: Subscribe FREE to our YouTube channel at https://www.youtube.com/c/cosmoquest Subscribe to our podcasts Astronomy Cast and Daily Space where ever you get your podcasts! Watch our streams over on Twitch at https://www.twitch.tv/cosmoquestx – follow and subscribe! Become a Patreon of CosmoQuest https://www.patreon.com/cosmoquestx Become a Patreon of Astronomy Cast https://www.patreon.com/astronomycast Buy stuff from our Redbubble https://www.redbubble.com/people/cosmoquestx Join our Discord server for CosmoQuest - https://discord.gg/X8rw4vv Join the Weekly Space Hangout Crew! - http://www.wshcrew.space/ Don't forget to like and subscribe! Plus we love being shared out to new people, so tweet, comment, review us... all the free things you can do to help bring science into people's lives.
The 365 Days of Astronomy, the daily podcast of the International Year of Astronomy 2009
https://youtu.be/b62FwfuM4SA Streamed live Dec 7th, 2022. Host: Fraser Cain ( @fcain ) Special Guest: During our November 16th show, Carolyn Collins Petersen introduced us to the hourglass/butterfly of L1527, an image captured by JWST using its onboard NIRCam. (You can read the original story here: https://www.nasa.gov/feature/goddard/...) This week we are joined by Dr. Karl Stapelfeldt, Chief Scientist for NASA's Exoplanet Exploration Program at JPL who will help us understand the science behind this amazing structure. Karl earned a B.S.E. in Aerospace Engineering and Engineering Physics at Princeton University, and a Ph.D. in Astrophysics at Caltech. His career at NASA includes positions at both the Jet Propulsion Laboratory and most recently at the Goddard Space Flight Center, where he has served as the Chief of Goddard's Exoplanets and Stellar Astrophysics Laboratory since 2011. Karl's NASA science contributions include project science roles for the Hubble and Spitzer Space Telescopes and science observations using the Herschel Space Observatory. He served as chair of the Exoplanet-Coronagraph Probe-Scale Science and Technology Definition Team, and as a member of the Astrophysics Subcommittee of the NASA Advisory Council. Regular Guests: Dr. Leah Jenks ( https://leahjenks.com/ / @leahgjenks ) Dr. Paul Byrne ( @ThePlanetaryGuy / https://eps.wustl.edu/people/paul-byrne ) This week's stories: - More updates from Artemis 1. - An asymmetry detected in the distribution of galaxies. - Mars occulted by the Moon! - A bizarre gamma ray burst that breaks all the rules! 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.
JWST NIRCam Defocused Imaging: Photometric Stability Performance and How it Can Sense Mirror Tilts by Everett Schlawin et al. on Wednesday 30 November We use JWST NIRCam short wavelength photometry to capture a transit lightcurve of the exoplanet HAT-P-14 b to assess performance as part of instrument commissioning. The short wavelength precision is 152 ppm per 27 second integration as measured over the full time series compared to a theoretical limit of 107 ppm, after corrections to spatially correlated 1/f noise. Persistence effects from charge trapping are well fit by an exponential function with short characteristic timescales, settling on the order of 5-15 minutes. The short wavelength defocused photometry is also uniquely well suited to measure the realtime wavefront error of JWST. Analysis of the images and reconstructed wavefront maps indicate that two different hexagonal primary mirror segments exhibited "tilt events" where they changed orientation rapidly in less than ~1.4 seconds. In some cases, the magnitude and timing of the flux jumps caused by tilt events can be accurately predicted with a telescope model. These tilt events can be sensed by simultaneous longer-wavelength NIRCam grism spectral images alone in the form of changes to the point spread function, diagnosed from the FWHM. They can also be sensed with the FGS instrument from difference images. Tilt events possibly from sudden releases of stress in the backplane structure behind the mirrors were expected during the commissioning period because they were found in ground-based testing. Tilt events have shown signs of decreasing in frequency but have not disappeared completely. The detectors exhibit some minor (less than 1%) deviations from linear behavior in the first few groups of each integration, potentially impacting absolute fluxes and transit depths on bright targets where only a handful of groups are possible. Overall, the noise is within 50% of the theoretical photon noise and read noise. This bodes well for high precision time series measurements. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16727v1
EIGER III JWST NIRCam observations of the ultra-luminous high-redshift quasar J0100+2802 by Anna-Christina Eilers et al. on Wednesday 30 November We present the first rest-frame optical spectrum of a high-redshift quasar observed with JWST/NIRCam in Wide Field Slitless (WFSS) mode. The observed quasar, J0100+2802, is the most luminous quasar known at $z>6$. We measure the mass of the central supermassive black hole (SMBH) by means of the rest-frame optical H$beta$ emission line, and find consistent mass measurements of the quasar's SMBH of $M_bulletapprox10^{10},M_odot$ when compared to the estimates based on the properties of rest-frame UV emission lines CIV and MgII, which are accessible from ground-based observatories. To this end, we also present a newly reduced rest-frame UV spectrum of the quasar observed with X-Shooter/VLT and FIRE/Magellan for a total of 16.8 hours. We readdress the question whether this ultra-luminous quasar could be effected by strong gravitational lensing making use of the diffraction limited NIRCam images in three different wide band filters (F115W, F200W, F356W), which improves the achieved spatial resolution compared to previous images taken with the Hubble Space Telescope by a factor of two. We do not find any evidence for a foreground deflecting galaxy, nor for multiple images of the quasar, and determine the probability for magnification due to strong gravitational lensing with image separations below the diffraction limit of $Deltathetalesssim 0.05''$ to be $lesssim 2.2times 10^{-3}$. Our observations therefore confirm that this quasar hosts a ten billion solar mass black hole less than $1$ Gyr after the Big Bang, which is challenging to explain with current black hole formation models. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16261v1
EIGER III JWST NIRCam observations of the ultra-luminous high-redshift quasar J0100+2802 by Anna-Christina Eilers et al. on Wednesday 30 November We present the first rest-frame optical spectrum of a high-redshift quasar observed with JWST/NIRCam in Wide Field Slitless (WFSS) mode. The observed quasar, J0100+2802, is the most luminous quasar known at $z>6$. We measure the mass of the central supermassive black hole (SMBH) by means of the rest-frame optical H$beta$ emission line, and find consistent mass measurements of the quasar's SMBH of $M_bulletapprox10^{10},M_odot$ when compared to the estimates based on the properties of rest-frame UV emission lines CIV and MgII, which are accessible from ground-based observatories. To this end, we also present a newly reduced rest-frame UV spectrum of the quasar observed with X-Shooter/VLT and FIRE/Magellan for a total of 16.8 hours. We readdress the question whether this ultra-luminous quasar could be effected by strong gravitational lensing making use of the diffraction limited NIRCam images in three different wide band filters (F115W, F200W, F356W), which improves the achieved spatial resolution compared to previous images taken with the Hubble Space Telescope by a factor of two. We do not find any evidence for a foreground deflecting galaxy, nor for multiple images of the quasar, and determine the probability for magnification due to strong gravitational lensing with image separations below the diffraction limit of $Deltathetalesssim 0.05''$ to be $lesssim 2.2times 10^{-3}$. Our observations therefore confirm that this quasar hosts a ten billion solar mass black hole less than $1$ Gyr after the Big Bang, which is challenging to explain with current black hole formation models. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16261v1
EIGER III JWST NIRCam observations of the ultra-luminous high-redshift quasar J0100+2802 by Anna-Christina Eilers et al. on Wednesday 30 November We present the first rest-frame optical spectrum of a high-redshift quasar observed with JWST/NIRCam in Wide Field Slitless (WFSS) mode. The observed quasar, J0100+2802, is the most luminous quasar known at $z>6$. We measure the mass of the central supermassive black hole (SMBH) by means of the rest-frame optical H$beta$ emission line, and find consistent mass measurements of the quasar's SMBH of $M_bulletapprox10^{10},M_odot$ when compared to the estimates based on the properties of rest-frame UV emission lines CIV and MgII, which are accessible from ground-based observatories. To this end, we also present a newly reduced rest-frame UV spectrum of the quasar observed with X-Shooter/VLT and FIRE/Magellan for a total of 16.8 hours. We readdress the question whether this ultra-luminous quasar could be effected by strong gravitational lensing making use of the diffraction limited NIRCam images in three different wide band filters (F115W, F200W, F356W), which improves the achieved spatial resolution compared to previous images taken with the Hubble Space Telescope by a factor of two. We do not find any evidence for a foreground deflecting galaxy, nor for multiple images of the quasar, and determine the probability for magnification due to strong gravitational lensing with image separations below the diffraction limit of $Deltathetalesssim 0.05''$ to be $lesssim 2.2times 10^{-3}$. Our observations therefore confirm that this quasar hosts a ten billion solar mass black hole less than $1$ Gyr after the Big Bang, which is challenging to explain with current black hole formation models. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16261v1
JWST NIRCam Observations of Stars and HII Regions in z simeq 6-8 Galaxies: Properties of Star Forming Complexes on 150 pc Scales by Zuyi Chen et al. on Tuesday 29 November The onset of the {it JWST}-era provides a much-improved opportunity to characterize the resolved structure of early star forming systems. Previous {it Spitzer} observations of $zgtrsim 6$ galaxies revealed the presence of old stars and luminous HII regions (via [OIII]+H$beta$ emission), but the poor resolution stunted our ability to map their locations with respect to the star forming regions identified in the rest-UV. In this paper, we investigate the internal structure of 12 of the most luminous $zsimeq 6-8$ galaxies in the EGS field observed with recent {it JWST}/NIRCam imaging. The systems appear clumpy in the rest-UV, with more than half of the light coming from $simeq 10^7$ to 10$^{9}$ M$_odot$ star forming complexes that are $simeq 150$ - 480 pc in size. The clumps tend to be dominated by young stars (median = 36 Myr), but we also find large variations in clump ages within individual galaxies. The [OIII]+H$beta$ EW varies significantly across individual galaxies (reflecting differences in stellar and gas properties), but the HII regions largely track the UV-bright complexes. Perhaps surprisingly, the rest-optical continuum is just as clumpy as the UV, and we do not find older (and redder) nuclear stellar components that were previously undetected or faint in the UV. The majority of the stellar mass in bright $6
First detections of stellar light from quasar host galaxies at z > 6 by Xuheng Ding et al. on Tuesday 29 November The existence of high-redshift supermassive black holes (SMBHs) -- shining brightly as quasars during the first billion years of our universe -- presents a conundrum in astrophysics. A broad variety of physical mechanisms have been proposed for the formation and rapid growth of these early SMBHs. Promising diagnostics are the relative properties of the black hole and its host galaxy. However, up to now, the detection of stars in quasar host galaxies has been elusive beyond $z>2$, even with deep HST observations. Here, we report the first detections of the stellar component of the host galaxies of two relatively low-luminosity quasars at $z>6$ observed with JWST using NIRCam. After modeling and subtracting the glare from the quasar itself, we find that the host galaxies are massive (stellar mass of $2.5times$ and $6.3times10^{10}$ M$_{odot}$), compact, and disk-like. Unlike most SMBHs in the nearby universe, these quasars are displaced from the centers of their host galaxies in the rest-frame optical, in one case by $0.9$ kpc. These first positive detections of quasar hosts at $z>6$ are a pivotal milestone; we can now assess the stellar environment along with star formation and black hole accretion to determine the physical conditions that govern the formation and evolution of the first SMBHs. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.14329v1
First detections of stellar light from quasar host galaxies at z > 6 by Xuheng Ding et al. on Monday 28 November The existence of high-redshift supermassive black holes (SMBHs) -- shining brightly as quasars during the first billion years of our universe -- presents a conundrum in astrophysics. A broad variety of physical mechanisms have been proposed for the formation and rapid growth of these early SMBHs. Promising diagnostics are the relative properties of the black hole and its host galaxy. However, up to now, the detection of stars in quasar host galaxies has been elusive beyond $z>2$, even with deep HST observations. Here, we report the first detections of the stellar component of the host galaxies of two relatively low-luminosity quasars at $z>6$ observed with JWST using NIRCam. After modeling and subtracting the glare from the quasar itself, we find that the host galaxies are massive (stellar mass of $2.5times$ and $6.3times10^{10}$ M$_{odot}$), compact, and disk-like. Unlike most SMBHs in the nearby universe, these quasars are displaced from the centers of their host galaxies in the rest-frame optical, in one case by $0.9$ kpc. These first positive detections of quasar hosts at $z>6$ are a pivotal milestone; we can now assess the stellar environment along with star formation and black hole accretion to determine the physical conditions that govern the formation and evolution of the first SMBHs. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.14329v1
Early Results From GLASS-JWST XVII: Building the First Galaxies -- Chapter 1 Star Formation Histories at 5
First Batch of Candidate Galaxies at Redshifts 11 to 20 Revealed by the James Webb Space Telescope Early Release Observations by Haojing Yan et al. on Monday 28 November On July 13, 2022, NASA released to the whole world the data obtained by the James Webb Space Telescope (JWST) Early Release Observations (ERO). These are the first set of science-grade data from this long-awaited facility, marking the beginning of a new era in astronomy. In the study of the early universe, JWST will allow us to push far beyond z ~ 11, the redshift boundary previously imposed by the 1.7 um red cut-off of the Hubble Space Telescope (HST). In contrast, JWST's NIRCam reaches 5 um. Among the JWST ERO targets there is a nearby galaxy cluster SMACS 0723-73, which is a massive cluster and has been long recognized as a potential "cosmic telescope" in amplifying background galaxies. The ERO six-band NIRCam observations on this target have covered an additional flanking field not boosted by gravitational lensing, which also sees far beyond HST. Here we report the result from our search of candidate objects at z > 11 using these ERO data. In total, there are 87 such objects identified by using the standard "dropout" technique. These objects are all detected in multiple bands and therefore cannot be spurious. For most of them, their multi-band colors are inconsistent with known types of contaminants. If the detected dropout signature is interpreted as the expected Lyman-break, it implies that these objects are at z ~ 11--20. The large number of such candidate objects at such high redshifts is not expected from the previously favored predictions and demands further investigations. JWST spectroscopy on such objects will be critical. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2207.11558v2
An Hα Impression of Lyα Galaxies at z simeq6 with Deep JWST NIRCam Imaging by Yuanhang Ning et al. on Monday 28 November We present a study of seven spectroscopically confirmed Ly{alpha} emitting galaxies at redshift $zsimeq6$ using the James Webb Space Telescope (JWST) NIRCam images. These galaxies, with a wide range of Ly{alpha} luminosities, were recently observed in a series of NIRCam broad- and medium-bands. We measure the continuum and H{alpha} line properties of the galaxies using the combination of the NIRCam photometry and archival Hubble Space Telescope imaging data. We find that galaxies with bluer UV continuum slopes likely have higher escape fractions of Ly{alpha} photons. We also find that galaxies with higher Ly{alpha} line emission tend to produce ionizing photons more efficiently. The most Ly{alpha}-luminous galaxy in the sample has a high ionizing photon production efficiency of log$_{10} xi_{rm ion, 0}$ (Hz erg$^{-1}$) > 26. Our results support that Ly{alpha} galaxies may have served as an important contributor to the cosmic reionization. Blue and bright Ly{alpha} galaxies are also excellent targets for JWST follow-up spectroscopic observations. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13620v1
JWST NIRCam Observations of Stars and HII Regions in z simeq 6-8 Galaxies: Properties of Star Forming Complexes on 150 pc Scales by Zuyi Chen et al. on Monday 28 November The onset of the {it JWST}-era provides a much-improved opportunity to characterize the resolved structure of early star forming systems. Previous {it Spitzer} observations of $zgtrsim 6$ galaxies revealed the presence of old stars and luminous HII regions (via [OIII]+H$beta$ emission), but the poor resolution stunted our ability to map their locations with respect to the star forming regions identified in the rest-UV. In this paper, we investigate the internal structure of 12 of the most luminous $zsimeq 6-8$ galaxies in the EGS field observed with recent {it JWST}/NIRCam imaging. The systems appear clumpy in the rest-UV, with more than half of the light coming from $simeq 10^7$ to 10$^{9}$ M$_odot$ star forming complexes that are $simeq 150$ - 480 pc in size. The clumps tend to be dominated by young stars (median = 36 Myr), but we also find large variations in clump ages within individual galaxies. The [OIII]+H$beta$ EW varies significantly across individual galaxies (reflecting differences in stellar and gas properties), but the HII regions largely track the UV-bright complexes. Perhaps surprisingly, the rest-optical continuum is just as clumpy as the UV, and we do not find older (and redder) nuclear stellar components that were previously undetected or faint in the UV. The majority of the stellar mass in bright $6
An Hα Impression of Lyα Galaxies at z simeq6 with Deep JWST NIRCam Imaging by Yuanhang Ning et al. on Sunday 27 November We present a study of seven spectroscopically confirmed Ly{alpha} emitting galaxies at redshift $zsimeq6$ using the James Webb Space Telescope (JWST) NIRCam images. These galaxies, with a wide range of Ly{alpha} luminosities, were recently observed in a series of NIRCam broad- and medium-bands. We measure the continuum and H{alpha} line properties of the galaxies using the combination of the NIRCam photometry and archival Hubble Space Telescope imaging data. We find that galaxies with bluer UV continuum slopes likely have higher escape fractions of Ly{alpha} photons. We also find that galaxies with higher Ly{alpha} line emission tend to produce ionizing photons more efficiently. The most Ly{alpha}-luminous galaxy in the sample has a high ionizing photon production efficiency of log$_{10} xi_{rm ion, 0}$ (Hz erg$^{-1}$) > 26. Our results support that Ly{alpha} galaxies may have served as an important contributor to the cosmic reionization. Blue and bright Ly{alpha} galaxies are also excellent targets for JWST follow-up spectroscopic observations. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13620v1
Early Results From GLASS-JWST XVII: Building the First Galaxies -- Chapter 1 Star Formation Histories at 5
First Batch of Candidate Galaxies at Redshifts 11 to 20 Revealed by the James Webb Space Telescope Early Release Observations by Haojing Yan et al. on Sunday 27 November On July 13, 2022, NASA released to the whole world the data obtained by the James Webb Space Telescope (JWST) Early Release Observations (ERO). These are the first set of science-grade data from this long-awaited facility, marking the beginning of a new era in astronomy. In the study of the early universe, JWST will allow us to push far beyond z ~ 11, the redshift boundary previously imposed by the 1.7 um red cut-off of the Hubble Space Telescope (HST). In contrast, JWST's NIRCam reaches 5 um. Among the JWST ERO targets there is a nearby galaxy cluster SMACS 0723-73, which is a massive cluster and has been long recognized as a potential "cosmic telescope" in amplifying background galaxies. The ERO six-band NIRCam observations on this target have covered an additional flanking field not boosted by gravitational lensing, which also sees far beyond HST. Here we report the result from our search of candidate objects at z > 11 using these ERO data. In total, there are 87 such objects identified by using the standard "dropout" technique. These objects are all detected in multiple bands and therefore cannot be spurious. For most of them, their multi-band colors are inconsistent with known types of contaminants. If the detected dropout signature is interpreted as the expected Lyman-break, it implies that these objects are at z ~ 11--20. The large number of such candidate objects at such high redshifts is not expected from the previously favored predictions and demands further investigations. JWST spectroscopy on such objects will be critical. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2207.11558v2
The production of ionizing photons in UV-faint z~3-7 galaxies by Gonzalo Prieto-Lyon et al. on Thursday 24 November The demographics of the production and escape of ionizing photons from UV-faint early galaxies is a key unknown in discovering the primary drivers of reionization. With the advent of JWST it is finally possible to observe the rest-frame optical nebular emission from individual sub-L$^*$ z>3 galaxies to measure the production of ionizing photons, $xi_mathrm{ion}$. Here we study a sample of 380 z~3-7 galaxies spanning -23 0.5) in our sample, based on their photometric properties, even amongst the Lyman-alpha selected galaxies. This work demonstrates that considering the full distribution of $xi_mathrm{ion}$ across galaxy properties is important for assessing the primary drivers of reionization. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12548v1
The production of ionizing photons in UV-faint z~3-7 galaxies by Gonzalo Prieto-Lyon et al. on Wednesday 23 November The demographics of the production and escape of ionizing photons from UV-faint early galaxies is a key unknown in discovering the primary drivers of reionization. With the advent of JWST it is finally possible to observe the rest-frame optical nebular emission from individual sub-L$^*$ z>3 galaxies to measure the production of ionizing photons, $xi_mathrm{ion}$. Here we study a sample of 380 z~3-7 galaxies spanning -23 0.5) in our sample, based on their photometric properties, even amongst the Lyman-alpha selected galaxies. This work demonstrates that considering the full distribution of $xi_mathrm{ion}$ across galaxy properties is important for assessing the primary drivers of reionization. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12548v1
Early Release Science of the exoplanet WASP-39b with JWST NIRCam by Eva-Maria Ahrer et al. on Tuesday 22 November Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 $mu$m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H$_2$O in the atmosphere and place an upper limit on the abundance of CH$_4$. The otherwise prominent CO$_2$ feature at 2.8 $mu$m is largely masked by H$_2$O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100$times$ solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10489v1
Early Release Science of the exoplanet WASP-39b with JWST NIRCam by Eva-Maria Ahrer et al. on Tuesday 22 November Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 $mu$m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H$_2$O in the atmosphere and place an upper limit on the abundance of CH$_4$. The otherwise prominent CO$_2$ feature at 2.8 $mu$m is largely masked by H$_2$O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100$times$ solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10489v1
Early Release Science of the exoplanet WASP-39b with JWST NIRCam by Eva-Maria Ahrer et al. on Monday 21 November Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 $mu$m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H$_2$O in the atmosphere and place an upper limit on the abundance of CH$_4$. The otherwise prominent CO$_2$ feature at 2.8 $mu$m is largely masked by H$_2$O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100$times$ solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10489v1
JWST NIRCam Probes Young Star Clusters in the Reionization Era Sunrise Arc by E. Vanzella et al. on Monday 21 November Star cluster formation in the early universe and their contribution to reionization remains to date largely unconstrained. Here we present JWST/NIRCam imaging of the most highly magnified galaxy known at z ~ 6, the Sunrise arc. We identify six young massive star clusters (YMCs) with measured radii spanning ~ 20 pc down to ~ 1 pc (corrected for lensing magnification), estimated stellar masses of ~ $10^{(6-7)}$ Msun, and with ages 1-30 Myr based on SED fitting to photometry measured in 8 filters extending to rest-frame 7000A. The resulting stellar mass surface densities are higher than 1000 Msun pc$^{-2}$ (up to a few $10^5$ Msun pc$^{-2}$) and their inferred dynamical ages qualify the majority of these systems as gravitationally-bound stellar clusters. The star cluster ages map the progression of star formation along the arc, with to evolved systems (>~ 10 Myr old) followed by very young clusters. The youngest stellar clusters (< 5 Myr) show evidence of prominent Hbeta + [OIII]4959,5007 emission, based on photometry, with equivalent widths larger than 1000 A rest-frame, and are hosted in a 200 pc sized star-forming complex. Such a region dominates the ionizing photon production, with a high efficiency log($xi_{ion}$ [Hz erg$^{-1}$]) ~ 25.7. A significant fraction of the recently formed stellar mass of the galaxy (> 10-30 %) occurred in these YMCs. We speculate that such sources of ionizing radiation boost the ionizing photon production efficiency which eventually carve ionized channels that might favor the escape of Lyman continuum radiation. The survival of some of the clusters would make them the progenitors of massive and relatively metal-poor globular clusters in the local Universe. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.09839v1
Early Release Science of the exoplanet WASP-39b with JWST NIRCam by Eva-Maria Ahrer et al. on Monday 21 November Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST's Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 - 4.0 $mu$m, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet's spectrum. Specifically, we detect gaseous H$_2$O in the atmosphere and place an upper limit on the abundance of CH$_4$. The otherwise prominent CO$_2$ feature at 2.8 $mu$m is largely masked by H$_2$O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1-100$times$ solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation or disequilibrium processes in the upper atmosphere. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10489v1
Hubble 太空望遠鏡 上有名 ê 一張相片 是：創生之柱。伊是鴟鴞星雲 M16 內底，ùi 冷氣體塗粉組成--ê、1 光年長--ê 恆星形成柱。毋過這張是 James Webb 太空望遠鏡 ê NIRCam 影像，有通看著 Hubble 進前看袂著 ê 部份，包括 tī 這个有名 ê 恆星托兒所內底，看著較濟細節 kah 較深空 ê 景色。佇 Webb 近紅外線景色內底上特別--ê，是佇雲柱上尾節 ê 紅色發射線。佇遐 ê 物質當咧進行重力崩塌，未來會形成恆星。鴟鴞星雲 離咱有 6500 光年遠。這个大閣光 ê 發射星雲 tùi 雙筒千里鏡抑是細台天文望遠鏡來講，是真好揣 ê 目標。M16 就佇咱銀河盤 ê 方向，遐是天頂厚星雲 ê 所在，就佇 分做兩爿--ê 巨蛇座尾溜遐。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20221020/ 影像來源：科學：NASA, ESA, CSA, STScI, NIRCam 資料處理：Joseph DePasquale (STScI), Anton M. Koekemoer (STScI), Alyssa Pagan (STScI) 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NCU) 原文：https://apod.nasa.gov/apod/ap221020.html Powered by Firstory Hosting
Historic Firsts: Arizona and the James Webb Telescope E31 On December 25, 2021, NASA launched the James Webb Space Telescope (JWST), the largest and most complex space telescope ever built. Four days later, Webb's massive sunshield deployed and within weeks, its primary mirror started unfurling. On August 12, 2022, Webb’s first images were released, and […] The post Historic Firsts: Arizona and the James Webb Telescope E31 appeared first on Business RadioX ®.
這張足清楚 ê 近紅外線相片是 James Webb 太空望遠鏡 翕--ê，中央有翕著 有環 ê 冰巨行星，海王星。這个暗淡 ê 遙遠世界是 離太陽上遠 ê 行星，差不多是地球到太陽距離 ê 30 倍遠。毋閣 tī 這个精彩 ê Webb 影像內底，這粒行星 暗甲親像是幽靈仝款，這是因為大氣層內底 ê 甲烷 kā 紅外線吸收了了。海王星表面大部份會吸收甲烷，伊頂懸 ê 懸雲，tī 這張相片內底嘛足明顯--ê。海王星上大粒 ê 衛星 海衛一 Triton 就 tī 這張 Webb 影像倒爿頂懸 ê 繞射光尖 遐。因為伊 ê 表面是堅凍 ê 窒素，所以伊比海王星反射太陽光閣較光。這張相片內底有 去 hŏng 揣著 海王星 14 粒衛星 ê 其中七粒，嘛包括海衛一 Triton。海王星 ê 環無遐爾光，伊就 tī 這張新翕--ê 太空行星肖像內底。這个複合環系統，是頭一擺翕甲遮爾清楚。頂擺翕著伊--ê，是 1989 年 8 月 ê 航海家 2 號太空船。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20220923/ 影像：NASA, ESA, CSA, STScI, NIRCam 音樂：高小糕 GaoXiaoGao 聲優：阿錕 翻譯：An-Li Tsai (NCU) 原文：https://apod.nasa.gov/apod/ap220923.html Powered by Firstory Hosting
JWST's PEARLS: A JWST NIRCam view of ALMA sources by Cheng Cheng et al. on Monday 17 October We report the results of James Webb Space Telescope/NIRCam observations of 19 (sub)millimeter (submm/mm) sources detected by the Atacama Large Millimeter Array (ALMA). The accurate ALMA positions allowed unambiguous identifications of their NIRCam counterparts. Taking gravitational lensing into account, these represent 16 distinct galaxies in three fields and constitute the largest sample of its kind to date. The counterparts' spectral energy distributions from rest-frame ultraviolet to near infrared provide photometric redshifts ($1
A First Look at Cepheids in a SN Ia Host with JWST by Wenlong Yuan et al. on Tuesday 20 September We report the first look at extragalactic Cepheid variables with the James Webb Space Telescope, obtained from a serendipitous (to this purpose) observation of NGC 1365, host of an SN Ia (SN 2012fr), a calibration path used to measure the Hubble constant. As expected, the high-resolution observations with NIRCam through F200W show better source separation from line-of-sight companions than HST images at similar near-infrared wavelengths, the spectral region that has been used to mitigate the impact of host dust on distance measurements. Using the standard star P330E as a zeropoint and PSF reference, we photometered 31 previously-known Cepheids in the JWST field, spanning 1.15 < log P < 1.75 including 24 Cepheids in the longer period interval of 1.35 < log P < 1.75. We compared the resultant Period-Luminosity relations to that of 49 Cepheids in the full period range including 38 in the longer period range observed with WFC3/IR on HST and transformed to the JWST photometric system (F200W, Vega). The P-L relations measured with the two space telescopes are in good agreement, with intercepts (at log P=1) of 25.74+/-0.04 and 25.72+-0.05 for HST and JWST, respectively. Our baseline result comes from the longer period range where the Cepheids have higher signal-to-noise ratios where we find 25.75+-0.05 and 25.75+-0.06 mag for HST and JWST, respectively. We find good consistency between this first JWST measurement and HST, and no evidence that HST Cepheid photometry is "biased bright" at the ~0.2 mag level that would be needed to mitigate the Hubble Tension, though comparisons from more SN hosts are warranted and anticipated. We expect future JWST observations to surpass these in quality as they will be optimized for measuring Cepheids. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09101v1
A First Look at Cepheids in a SN Ia Host with JWST by Wenlong Yuan et al. on Tuesday 20 September We report the first look at extragalactic Cepheid variables with the James Webb Space Telescope, obtained from a serendipitous (to this purpose) observation of NGC 1365, host of an SN Ia (SN 2012fr), a calibration path used to measure the Hubble constant. As expected, the high-resolution observations with NIRCam through F200W show better source separation from line-of-sight companions than HST images at similar near-infrared wavelengths, the spectral region that has been used to mitigate the impact of host dust on distance measurements. Using the standard star P330E as a zeropoint and PSF reference, we photometered 31 previously-known Cepheids in the JWST field, spanning 1.15 < log P < 1.75 including 24 Cepheids in the longer period interval of 1.35 < log P < 1.75. We compared the resultant Period-Luminosity relations to that of 49 Cepheids in the full period range including 38 in the longer period range observed with WFC3/IR on HST and transformed to the JWST photometric system (F200W, Vega). The P-L relations measured with the two space telescopes are in good agreement, with intercepts (at log P=1) of 25.74+/-0.04 and 25.72+-0.05 for HST and JWST, respectively. Our baseline result comes from the longer period range where the Cepheids have higher signal-to-noise ratios where we find 25.75+-0.05 and 25.75+-0.06 mag for HST and JWST, respectively. We find good consistency between this first JWST measurement and HST, and no evidence that HST Cepheid photometry is "biased bright" at the ~0.2 mag level that would be needed to mitigate the Hubble Tension, though comparisons from more SN hosts are warranted and anticipated. We expect future JWST observations to surpass these in quality as they will be optimized for measuring Cepheids. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09101v1
Early Results From GLASS-JWST XII: The Morphology of Galaxies at the Epoch of Reionization by T. Treu et al. on Monday 19 September Star-forming galaxies can exhibit strong morphological differences between the rest-frame far-UV and optical, reflecting inhomogeneities in star-formation and dust attenuation. We exploit deep, high resolution NIRCAM 7-band observations to take a first look at the morphology of galaxies in the epoch of reionization ($z>7$), and its variation in the rest-frame wavelength range between Lyman $alpha$ and 6000-4000AA, at $z=7-12$. We find no dramatic variations in morphology with wavelength -- of the kind that would have overturned anything we have learned from the Hubble Space Telescope. No significant trends between morphology and wavelengths are detected using standard quantitative morphology statistics. We detect signatures of mergers/interactions in 4/19 galaxies. Our results are consistent with a scenario in which Lyman Break galaxies -- observed when the universe is only 400-800 Myrs old - are growing via a combination of rapid galaxy-scale star formation supplemented by accretion of star forming clumps and interactions. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2207.13527v2
Photometry and astrometry with JWST -- I NIRCam Point Spread Functions and the first JWST colour-magnitude diagrams of a globular cluster by D. Nardiello et al. on Wednesday 14 September As the James Webb Space Telescope (JWST) has become fully operational, early-release data are now available to begin building the tools and calibrations for precision point-source photometry and astrometry in crowded cluster environments. Here, we present our independent reduction of NIRCam imaging of the metal-poor globular cluster M92, which were collected under Director's Discretionary Early Release Science programme ERS-1334. We derived empirical models of the Point Spread Function (PSF) for filters F090W, F150W, F277W, and F444W, and find that these PSFs: (i) are generally under-sampled (FWHM~2 pixel) in F150W and F444W and severely under-sampled (FWHM~1 pixel) in F090W and F277W; (ii) have significant variation across the field of view, up to ~15-20 %; and (iii) have temporal variations of ~3-4 % across multi-epoch exposures. We deployed our PSFs to determine the photometric precision of NIRCam for stars in the crowded, central regions of M92, measured to be at the ~0.01 mag level. We use these data to construct the first JWST colour-magnitude diagrams of a globular cluster. Employing existing stellar models, we find that the data reach almost the bottom of the M92 main sequence (~0.1 M$_{odot}$), and reveal 24 white dwarf candidate members of M92 in the brightest portion of the white dwarf cooling sequence. The latter are confirmed through a cross-match with archival HST UV and optical data. We also detect the presence of multiple stellar populations along the low-mass main sequence of M92. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.06547v1
GOALS-JWST: NIRCam and MIRI Imaging of the Circumnuclear Starburst Ring in NGC 7469 by Thomas Bohn et al. on Monday 12 September We present James Webb Space Telescope (JWST) imaging of NGC 7469 with the Near-Infrared Camera (NIRCam) and the Mid-InfraRed Instrument (MIRI). NGC 7469 is a nearby, $z=0.016317$, luminous infrared galaxy (LIRG) that hosts both a Seyfert Type-1.5 nucleus and a circumnuclear starburst ring with a radius of $sim$0.5 kpc. The new near-infrared (NIR) JWST imaging reveals 65 star-forming regions, 36 of which were not detected by HST observations. Nineteen of the 36 sources have very red NIR colors that indicate obscurations up to A$_{rm{v}}sim7$ and a contribution of at least 25$%$ from hot dust emission to the 4.4$mu$m band. Their NIR colors are also consistent with young ($
Performance of near-infrared high-contrast imaging methods with JWST from commissioning by Jens Kammerer et al. on Sunday 11 September The James Webb Space Telescope (JWST) will revolutionize the field of high-contrast imaging and enable both the direct detection of Saturn-mass planets and the characterization of substellar companions in the mid-infrared. While JWST will feature unprecedented sensitivity, angular resolution will be the key factor when competing with ground-based telescopes. Here, we aim to characterize the performance of several extreme angular resolution imaging techniques available with JWST in the 3-5 micron regime based on data taken during commissioning. Firstly, we introduce custom tools to simulate, reduce, and analyze NIRCam and MIRI coronagraphy data and use these tools to extract companion detection limits from on-sky NIRCam round and bar mask coronagraphy observations. Secondly, we present on-sky NIRISS aperture masking interferometry (AMI) and kernel phase imaging (KPI) observations from which we extract companion detection limits using the publicly available fouriever tool. Scaled to a total integration time of one hour and a target of the brightness of AB Dor, we find that NIRISS AMI and KPI reach contrasts of $sim$7-8 mag at $sim$70 mas and $sim$9 mag at $sim$200 mas. Beyond $sim$250 mas, NIRCam coronagraphy reaches deeper contrasts of $sim$13 mag at $sim$500 mas and $sim$15 mag at $sim$2 arcsec. While the bar mask performs $sim$1 mag better than the round mask at small angular separations $lesssim$0.75 arcsec, it is the other way around at large angular separations $gtrsim$1.5 arcsec. Moreover, the round mask gives access to the full 360 deg field-of-view which is beneficial for the search of new companions. We conclude that already during the instrument commissioning, JWST high-contrast imaging in the L- and M-bands performs close to its predicted limits. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.00996v3
Performance of near-infrared high-contrast imaging methods with JWST from commissioning by Jens Kammerer et al. on Sunday 11 September The James Webb Space Telescope (JWST) will revolutionize the field of high-contrast imaging and enable both the direct detection of Saturn-mass planets and the characterization of substellar companions in the mid-infrared. While JWST will feature unprecedented sensitivity, angular resolution will be the key factor when competing with ground-based telescopes. Here, we aim to characterize the performance of several extreme angular resolution imaging techniques available with JWST in the 3-5 micron regime based on data taken during commissioning. Firstly, we introduce custom tools to simulate, reduce, and analyze NIRCam and MIRI coronagraphy data and use these tools to extract companion detection limits from on-sky NIRCam round and bar mask coronagraphy observations. Secondly, we present on-sky NIRISS aperture masking interferometry (AMI) and kernel phase imaging (KPI) observations from which we extract companion detection limits using the publicly available fouriever tool. Scaled to a total integration time of one hour and a target of the brightness of AB Dor, we find that NIRISS AMI and KPI reach contrasts of $sim$7-8 mag at $sim$70 mas and $sim$9 mag at $sim$200 mas. Beyond $sim$250 mas, NIRCam coronagraphy reaches deeper contrasts of $sim$13 mag at $sim$500 mas and $sim$15 mag at $sim$2 arcsec. While the bar mask performs $sim$1 mag better than the round mask at small angular separations $lesssim$0.75 arcsec, it is the other way around at large angular separations $gtrsim$1.5 arcsec. Moreover, the round mask gives access to the full 360 deg field-of-view which is beneficial for the search of new companions. We conclude that already during the instrument commissioning, JWST high-contrast imaging in the L- and M-bands performs close to its predicted limits. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.00996v3
Webb's PEARLS: Bright 1 5--2 0 micron Dropouts in the Spitzer IRAC Dark Field by Haojing Yan et al. on Sunday 11 September Using the first epoch of four-band NIRCam observations obtained by the James Webb Space Telescope Prime Extragalactic Areas for Reionization and Lensing Science Program in the Spitzer IRAC Dark Field, we search for F150W and F200W dropouts following the conventional dropout method to select candidate objects at z>11. In 14.2 arcmin^2, we have found 13 F150W dropouts and 8 F200W dropouts, all brighter than 27.5 mag in the band to the red side of the break signature. Most notably, some of these objects are as bright as ~24 mag, which corresponds to M_{UV}11. As they are detected in multiple bands, these must be real objects. If the observed color decrements are due to the expected Lyman break, these objects should be at z>11.7 and z>15.4, respectively. The color diagnostics show that at least 11 F150W dropouts are far away from the usual contaminators encountered in dropout searches (red galaxies at much lower redshifts or brown dwarf stars), and therefore they are legitimate candidates. While the diagnostics of the F200W dropouts are less certain due to the limited number of passbands, at least one of them is not likely a known type of contaminant and the rest are consistent with either z>11 galaxies with evolved stellar populations or old galaxies at z ~ 3 to 8. If a significant fraction of our dropouts are indeed at z>11, we have to face the severe problem of explaining their high luminosities and number densities. Spectroscopic identifications of such objects are urgently needed. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04092v1
Webb's PEARLS: Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results by Rogier A. Windhorst et al. on Sunday 11 September We give an overview and describe the rationale, methods, and first results from NIRCam images of the JWST "Prime Extragalactic Areas for Reionization and Lensing Science" ("PEARLS") project. PEARLS uses up to eight NIRCam filters to survey several prime extragalactic survey areas: two fields at the North Ecliptic Pole (NEP); seven gravitationally lensing clusters; two high redshift proto-clusters; and the iconic backlit VV~191 galaxy system to map its dust attenuation. PEARLS also includes NIRISS spectra for one of the NEP fields and NIRSpec spectra of two high-redshift quasars. The main goal of PEARLS is to study the epoch of galaxy assembly, AGN growth, and First Light. Five fields, the JWST NEP Time-Domain Field (TDF), IRAC Dark Field (IDF), and three lensing clusters, will be observed in up to four epochs over a year. The cadence and sensitivity of the imaging data are ideally suited to find faint variable objects such as weak AGN, high-redshift supernovae, and cluster caustic transits. Both NEP fields have sightlines through our Galaxy, providing significant numbers of very faint brown dwarfs whose proper motions can be studied. Observations from the first spoke in the NEP TDF are public. This paper presents our first PEARLS observations, their NIRCam data reduction and analysis, our first object catalogs, the 0.9-4.5 $mu$m galaxy counts and Integrated Galaxy Light. We assess the JWST sky brightness in 13 NIRCam filters, yielding our first constraints to diffuse light at 0.9-4.5 $mu$m. PEARLS is designed to be of lasting benefit to the community. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04119v1
First Sample of H α + O III λ 5007 Line Emitters at z > 6 through JWST NIRCam Slitless Spectroscopy: Physical Properties and Line Luminosity Functions by Fengwu Sun et al. on Thursday 08 September We present a sample of four emission-line galaxies at $z=6.11-6.35$ that were serendipitously discovered using the commissioning data for the JWST/NIRCam wide-field slitless spectroscopy (WFSS) mode. One of them (at $z=6.11$) has been reported previously while the others are new discoveries. These sources are selected by the secure detections of both [O III] $lambda$5007 and H$alpha$ lines with other fainter lines tentatively detected in some cases (e.g., [O II] $lambda$3727, [O III] $lambda$4959 and [N II] $lambda$6583). In the [O III]/H$beta$ - [N II]/H$alpha$ Baldwin-Phillips-Terlevich diagram, these galaxies occupy the same parameter space as that of $zsim2$ star-forming galaxies, indicating that they have been enriched rapidly to sub-solar metallicities ($sim$0.6 $Z_{odot}$), similar to galaxies with comparable stellar masses at much lower redshifts. The detection of strong H$alpha$ lines suggests a higher ionizing photon production efficiency within galaxies in the early Universe. We find brightening of the [O III] $lambda$5007 line luminosity function (LF) from $z=3$ to 6, and no or weak redshift evolution of the H$alpha$ line LF from $z=2$ to 6. Both LFs are under-predicted at $zsim6$ by a factor of $sim$10 in certain cosmological simulations. This further indicates a global Ly$alpha$ photon escape fraction of 5-7% at $zsim6$, much lower than previous estimates through the comparison of the UV-derived star-formation rate density and Ly$alpha$ luminosity density. Our sample recovers $88^{+164}_{-57}$% of $z=6.0-6.6$ galaxies in the survey volume with stellar masses greater than $5times10^8$ $M_{odot}$, suggesting the ubiquity of strong H$alpha$ and [O III] line emitters in the Epoch of Reionization, which will be further uncovered in the era of JWST. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03374v1
Early results from GLASS-JWST V: the first rest-frame optical size-luminosity relation of galaxies at z>7 by Lilan Yang et al. on Wednesday 07 September We present the first rest-frame optical size-luminosity relation of galaxies at $z>7$, using the NIRCam imaging data obtained by the GLASS James Webb Space Telescope Early Release Science (GLASS-JWST-ERS) program, providing the deepest extragalactic data of the ERS campaign. Our sample consist of 19 photometrically selected bright galaxies with $m_text{F444W}leq27.8$ at $7
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Show Notes: Researchers discover new way fat cells talk directly with the brain | New Atlas (01:36) Researchers at the Scripps Research Institute have discovered a novel communication pathway between fat cells and the brain. Brain doesn't regulate fat burning by just slowly responding to hormonal signals in the blood. (traditional view) But can directly send messages to fat tissue and influence metabolic processes. The researchers use 2 new ways of looking at the fat tissue: 1. HYBRiD - This method renders fat tissue transparent, allowing researchers a unique window into the paths of neurons. 2. ROOT, and it lets the researchers study exactly how certain neurons localized in fat tissue communicate with other parts of the body. The big finding from the study was the discovery of sensory neurons that branch out from the spine into fat tissue. Directly communicate with a part of the brain called the dorsal root ganglia. Co-senior author Li Ye, stated on this finding: “The discovery of these neurons suggests for the first time that your brain is actively surveying your fat, rather than just passively receiving messages about it … The implications of this finding are profound.” Researchers found by blocking communication from these sensory neurons the sympathetic nervous system kicked into gear and began converting the white fat cells into brown fat. Stepping up the body's fat-burning processes. All this finding can clearly establish at this stage is that the newly discovered sensory neuron communication pathway is crucial for keeping fat tissue healthy. Two-Seater eVTOL Will Be Used to Train Pilots for Flying Taxis | Singularity Hub (07:38) London-based SkyFly has recently started taking pre-orders on a personal eVTOL called the Axe. It seats two, different the others trying to hit the market (seat one) Unlike its peers, the Axe has a fixed-wing design, so it's able to take off and land both vertically and in the conventional way. Vertical takeoff: Four propellers (4 ft diameter) lifts it off the ground, and once airborne, the body tilts forward to gain speed. Eight 35-kilowatt electric engines power the plane Mounted at a 45-degree angle and don't rotate. Wingspan is 16.4 feet Larger than any of the other personal aircraft Weighs 944 pounds (lithium battery pack accounts for a good portion of that total) Lift a maximum weight of 379 pounds. Its top speed is 100 miles per hour, and its range is 100 miles (200 if you add an optional range extender). Skyfly is aiming for its customer base to be made up of people who are already licensed pilots and/or own their own aircraft, and those who want to become pilots. Right now there's not only a shortage of pilots for commercial aircraft, there's not a cost-effective way to train new pilots either. And Skyfly CEO Michael Thompson wants the Axe to serve as a general aviation platform for pilots in training. SkyFly is taking pre-orders at a base price of US$175k. The company is planning to start production in 2024. A Simple Way to Produce Hydrogen From Water at Room Temperature | ScienceAlert (15:52) A new study out of University of California, Santa Cruz (UCSC), provides us with another promising step in Hydrogen clean fuel, provided you can make use of existing supplies of post-consumer aluminum and gallium. Discovered a simple method involving aluminum nanoparticles that are able to strip the oxygen from water molecules and leave hydrogen gas. yields large amounts of hydrogen, and it all works at room temperature. This discovery removes one of the big barriers to hydrogen fuel production: the large amounts of power required to produce it using existing methods. Works with any kind of water, too, including wastewater and ocean water. Materials scientist Scott Oliver from UCSC seemed surprised by this process: "We don't need any energy input, and it bubbles hydrogen like crazy … I've never seen anything like it.” With the help of scanning electron microscopy and X-ray diffraction techniques, the researchers were able to find the best mix of aluminum and gallium for producing hydrogen with the greatest efficiency. a 3:1 gallium-aluminum composite. Gallium is an expensive and less abundant material, but at least in this process it can be recovered and reused many times over without losing its effectiveness. Bakthan Singaram, a professor of organic chemistry at UCSC, stated: “The gallium separates the nanoparticles and keeps them from aggregating into larger particles … People have struggled to make aluminum nanoparticles, and here we are producing them under normal atmospheric pressure and room temperature conditions." There is still work to do, not least in making sure this can be scaled up from a lab set-up to something that can be used on an industrial scale. Promising sign for hydrogen fuel This Type of Supplement Can Reduce Depression and Anxiety | SciTechDaily (21:50) Researchers from the University of Reading studied the effects of high doses of Vitamin B6 on young adults. Felt less anxious and depressed after taking the supplements every day for a month. Adds to the body of evidence supporting the use of supplements believed to alter brain activity levels for the prevention or treatment of mood disorders. Dr. David Field, the lead author of the study explains: “The functioning of the brain relies on a delicate balance between the excitatory neurons that carry information around and inhibitory ones, which prevent runaway activity. Recent theories have connected mood disorders and some other neuropsychiatric conditions with a disturbance of this balance, often in the direction of raised levels of brain activity. Vitamin B6 helps the body produce a specific chemical messenger that inhibits impulses in the brain, and our study links this calming effect with reduced anxiety among the participants.” Vitamin B6 promotes the body's production of GABA (Gamma-Aminobutyric Acid), a molecule that blocks nerve cell impulses in the brain. Vitamin B12 was also looked at. Had little effect compared to placebo over the trial period. Vitamin B6 made a statistically reliable difference. Dr. Field talks on foods to consume, and more research that needs to be done: “Many foods, including tuna, chickpeas, and many fruits and vegetables, contain Vitamin B6. However, the high doses used in this trial suggest that supplements would be necessary to have a positive effect on mood. It is important to acknowledge that this research is at an early stage and the effect of Vitamin B6 on anxiety in our study was quite small compared to what you would expect from medication. However, nutrition-based interventions produce far fewer unpleasant side effects than drugs, and so in the future people might prefer them as an intervention.” James Webb Telescope captures its first images of an exoplanet | Interesting Engineering (28:30) In a first for the James Webb Telescope, astronomers from the joint NASA/ESA/CSA cooperative used the space-based telescope to bring back images of an exoplanet. Images of the exoplanet are seen through four different light filters These images lead the way toward future observations that can reveal a broad range of information never before seen on exoplanets. Exoplanet looked at was a gas giant, named HIP 65426 b, which is about six to eight times the size of Jupiter. Only about 15 to 20 million years old, which in planet years is very young Earth: is about four to five billion years old. These detailed images captured an exoplanet so well it is already leading to future possibilities for studying distant worlds. The Webb instrument captures light differently, and so the images have different presentations. Purple shows the NIRCam instruments view at 3.00 micrometers Blue shows the NIRCam instruments view at 4.44 micrometers Yellow images show the mid-infrared instrument's view at 11.4 micrometers. Red shows the mid-infrared instrument's view at 15.5 micrometers The difficulty in getting images of exoplanets is that the stars are so much brighter than planets. For instance, HIP 65426 b is more than 10,000 times fainter than its host star in the near-infrared, possibly 3,000 times fainter in the mid-infrared.
La tertulia semanal en la que repasamos las últimas noticias de la actualidad científica. En el episodio de hoy: El chorizo más famosa de la galaxia (min 7:00); Pospuesto el lanzamiento de Artemis I (28:00); Estructura en las secuencias vocales de los chimpancés (1:28:00); Galaxias no tan distantes, tras la calibración de NIRCam en JWST (2:25:00); ¿Tiene algún sentido eso de que se ha refutado el Big Bang? (2:35:00). Contertulios: María Ribes, Héctor Vives, Gastón Giribet, Sara Robisco, Alberto Aparici, Francis Villatoro, Héctor Socas. Portada gentileza de Manu Pombrol. Todos los comentarios vertidos durante la tertulia representan únicamente la opinión de quien los hace... y a veces ni eso. CB:SyR es una actividad del Museo de la Ciencia y el Cosmos de Tenerife. Museos de Tenerife apoya el valor científico y divulgativo de CB:SyR sin asumir como propios los comentarios de los participantes.
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High Contrast Imaging of the Exoplanet HIP 65426 b from 2-16 μ m by Aarynn L. Carter et al. on Thursday 01 September We present JWST Early Release Science (ERS) coronagraphic observations of the super-Jupiter exoplanet, HIP 65426 b, with the Near-Infrared Camera (NIRCam) from 2-5 $mu$m, and with the Mid-Infrared Instrument (MIRI) from 11-16 $mu$m. At a separation of $sim$0.82" (87$^{+108}_{-31}$ au), HIP 65426 b is clearly detected in all seven of our observational filters, representing the first images of an exoplanet to be obtained by JWST, and the first ever direct detection of an exoplanet beyond 5 $mu$m. These observations demonstrate that JWST is exceeding its nominal predicted performance by up to a factor of 10, with measured 5$sigma$ contrast limits of $sim$4$times10^{-6}$ ($sim$2.4 $mu$Jy) and $sim$2$times10^{-4}$ ($sim$10 $mu$Jy) at 1" for NIRCam at 3.6 $mu$m and MIRI at 11.3 $mu$m, respectively. These contrast limits provide sensitivity to sub-Jupiter companions with masses as low as 0.3 $M_mathrm{Jup}$ beyond separations of $sim$100 au. Together with existing ground-based near-infrared data, the JWST photometry are well fit by a BT-SETTL atmospheric model from 1-16 $mu$m, and span $sim$97% of HIP 65426 b's luminous range. Independent of the choice of forward model atmosphere we measure an empirical bolometric luminosity that is tightly constrained between $mathrm{log}!left(L_mathrm{bol}/L_{odot}right)$=-4.35 to -4.21, which in turn provides a robust mass constraint of 7.1$pm$1.1 $M_mathrm{Jup}$. In totality, these observations confirm that JWST presents a powerful and exciting opportunity to characterise the population of exoplanets amenable to direct imaging in greater detail. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.14990v2
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High Contrast Imaging of the Exoplanet HIP 65426 b from 2-16 μ m by Aarynn L. Carter et al. on Thursday 01 September We present JWST Early Release Science (ERS) coronagraphic observations of the super-Jupiter exoplanet, HIP 65426 b, with the Near-Infrared Camera (NIRCam) from 2-5 $mu$m, and with the Mid-Infrared Instrument (MIRI) from 11-16 $mu$m. At a separation of $sim$0.82" (87$^{+108}_{-31}$ au), HIP 65426 b is clearly detected in all seven of our observational filters, representing the first images of an exoplanet to be obtained by JWST, and the first ever direct detection of an exoplanet beyond 5 $mu$m. These observations demonstrate that JWST is exceeding its nominal predicted performance by up to a factor of 10, with measured 5$sigma$ contrast limits of $sim$4$times10^{-6}$ ($sim$2.4 $mu$Jy) and $sim$2$times10^{-4}$ ($sim$10 $mu$Jy) at 1" for NIRCam at 3.6 $mu$m and MIRI at 11.3 $mu$m, respectively. These contrast limits provide sensitivity to sub-Jupiter companions with masses as low as 0.3 $M_mathrm{Jup}$ beyond separations of $sim$100 au. Together with existing ground-based near-infrared data, the JWST photometry are well fit by a BT-SETTL atmospheric model from 1-16 $mu$m, and span $sim$97% of HIP 65426 b's luminous range. Independent of the choice of forward model atmosphere we measure an empirical bolometric luminosity that is tightly constrained between $mathrm{log}!left(L_mathrm{bol}/L_{odot}right)$=-4.35 to -4.21, which in turn provides a robust mass constraint of 7.1$pm$1.1 $M_mathrm{Jup}$. In totality, these observations confirm that JWST presents a powerful and exciting opportunity to characterise the population of exoplanets amenable to direct imaging in greater detail. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.14990v2
美麗 ê 捲螺仔星系 Messir 74 (嘛叫做 NGC 628) 就 chhāi tī 雙魚座 ê 方向，離咱有 3200 萬光年遠。M74 有兩支足大支 ê 捲螺仔手骨，這个島宇宙差不多有 1000 億粒恆星 tī 內底。長期以來，攏因為伊 ê 宏偉結構，煞去予天文學家 kā 伊當做是捲螺仔星系 ê 模範。這張是最近 ùi James Webb 太空望遠鏡 ê 公開觀測資料 處理 ê 影像，M74 ê 中央區清楚甲予人掣一趒。這張彩色 ê 合成影像是 ùi Webb 太空望遠鏡 ê 兩个儀器 NIRcam kah MIRI 來--ê。In 是 近紅外線 kah 中紅外線波段 ê kha-mé-lah。Tī 這个有宏偉結構 ê 捲螺仔星系影像內底，看會著較冷 ê 恆星 kah 塗粉結構，這攏是以前 ê 太空望遠鏡 看袂著--ê。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20220722/ 影像來源：NASA, ESA, CSA, STScI 資料處理 kah 版權: Robert Eder 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NCU) 原文：https://apod.nasa.gov/apod/ap220722.html Powered by Firstory Hosting
南環星雲是一个 行星形星雲，去予編做 NGC 3132。伊是一个離咱地球 2500 光年遠，欲死的類太陽恆星 ê 殮布。這張是 James Webb 太空望遠鏡 翕 ê 相片，無想到會當看著遮爾濟細節。內底有氣體 kah 塗粉組成、予人呵咾甲會觸舌 ê 宇宙天景，伊 ê 直徑是半光年長。Tī 這張 NIRCam 影像中心附近 足光彼粒恆星，是欲死的恆星 ê 星伴。這个互踅系統內底，較暗彼粒恆星，tī 過去幾若千年 ê 時間內，已經演化到 kā 星雲氣體塗粉殼擲出來 ê 階段矣。這粒較暗 ê 恆星就 tī 繞射光尖 ê 8 點鐘方向遐，落尾伊會演化做白矮星。這兩粒恆星 ê 互踅運動，就是造成南環星雲複雜結構 ê 原因。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20220714/ 影像：NASA, ESA, CSA, STScI, NIRCam 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NCU) 原文：https://apod.nasa.gov/apod/ap220714.html Powered by Firstory Hosting
這是目前為止 上深空、上清楚 ê 紅外線宇宙影像。是 James Webb 太空望遠鏡 面頂 ê NIRCam，開 12.5 點鐘久 ê 感光時間，tùi 南方星座飛魚座方向翕 ê 早期宇宙 景色。是講，相片內底有六條 繞射光針 ê 恆星，攏是咱銀河系內底 ê 恆星。這款 繞射 花樣，是 Webb 望遠鏡 ê 特徵。因為伊直徑 6.5 公尺 ê 主鏡，是 ùi 18 塊細塊六角鏡 鬥做一塊，做伙觀測--ê。視野內底幾若千个星系，攏是遠方 ê 星系團 SMACS0723-73 內底 ê 成員，差不多是 25 億光年遠。深空視野內底 ê 光弧，看起來敢若是 ùi 閣較遠 ê 星系來--ê。星系團 ê 主要質量是烏暗物質。影像去予 星系團 kā 扭曲 kah 放大--ê，這就叫做 重力 透鏡效應。Webb ê NIRISS 儀器表示講，kā 有光尖 ê 恆星後壁兩个無仝 ê 光弧資料 做分析，發現講這寡光弧攏是 ùi 仝一个背景星系來 ê 影像。而且這寡光，是愛開 95 億年 ê 時間，才行到 James Webb 太空望遠鏡。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20220713/ 影像：NASA, ESA, CSA, STScI, NIRCam 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NCU) 原文：https://apod.nasa.gov/apod/ap220713.html Powered by Firstory Hosting
A nursery of stars. Galaxies 13 billion light years away. The Carina Nebula. These are some of the spectacular images captured by the James Webb Telescope from its vantage point one million miles away from earth. As the telescope's detail-saturated pictures were beamed across the world on Tuesday, they were met with awed silence as well as whoops of joy from scientists, some whose entire careers have been dedicated to the telescope. One of the most complicated spacecraft ever launched, the the telescope, which boasts a sun shield the size of a tennis court, will beam back images and data for the next 20 years. We'll talk to scientists who helped design the James Webb Telescope and find out what we can expect to see next. Guests: Marcia Rieke, Regents' professor of Astronomy and astronomer, Steward Observatory, University of Arizona - Dr. Rieke is the principal investigator for the NIRCam on the James Webb Space Telescope. Tom Greene, astrophysicist, Space Science and Astrobiology Division at NASA Ames Research Center - Dr. Greene works on the NIRCam and MIRI science instruments on the James Webb Telescope. Marina Koren, staff writer, The Atlantic - Koren covers space for the magazine.
這个視野中心 ê 恆星 to̍h 叫做 2MASS J17554042+6551277。這實在是有夠歹讀 ê，毋閣這就是伊 ê 名，是用座標來做伊 ê 目錄編號。愛好遙遠宇宙 ê 迷眾，應該已經慣勢伊尖尖 ê 形體矣。這个繞射圖樣是 18 塊 六角鏡 鬥--出來 ê James Webb 太空望遠鏡 (JWST) 產生 ê。Kā 摺--起來 ê 望遠鏡拍開了後，逐塊細塊鏡會 調整到紅外線波段需要 ê 繞射極限，予 in 有法度當做是一塊直徑 6.5 公尺闊 ê 主鏡 來運作。Ùi 這个 Webb 望遠鏡 ê 近紅外線 kha-mé-lah (NIRcam) 翕 ê 相片看會出來，in 對齊 ê 精確度已經到目前 ê 物理極限 矣。2MASS J17554042+6551277 離咱才 2000 光年遠爾爾，猶 tī 咱 ê 銀河系內底。毋閣 tī Webb 望遠鏡 leh 做對齊評估 ê 影像內底，背景彼寡星系可能有幾若十億光年遠，彼 to̍h 比咱銀河閣較遠 矣。 ——— 這是 NASA Astronomy Picture of the Day ê 台語文 podcast 原文版：https://apod.nasa.gov/ 台文版：https://apod.tw/ 今仔日 ê 文章： https://apod.tw/daily/20220319/ 影像：NASA, STScI, JWST 音樂：P!SCO - 鼎鼎 聲優：阿錕 翻譯：An-Li Tsai (NCU) 原文：https://apod.nasa.gov/apod/ap220319.html Powered by Firstory Hosting
NIRCam which is attached to the James Webb Space Telescope. NIRCam will study infrared light and help astronomers learn the age of stars in nearby galaxies
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