DOCSLIB.ORG

NGC 1333 Plunkett Et

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
NGC 1333 Plunkett Et Outflows in protostellar clusters: a multi-wavelength, multi-scale view Adele L. Plunkett1, H. G. Arce1, S. A. Corder2, M. M. Dunham1, D. Mardones3 1-Yale University; 2-ALMA; 3-Universidad de Chile Interferometer and Single Dish Overview Combination FCRAO-only v=-2 to 6 km/s FCRAO-only v=10 to 17 km/s K km s While protostellar outflows are generally understood as necessary components of isolated star formation, further observations are -1 needed to constrain parameters of outflows particularly within protostellar clusters. In protostellar clusters where most stars form, outflows impact the cluster environment by injecting momentum and energy into the cloud, dispersing the surrounding gas and feeding turbulent motions. Here we present several studies of very dense, active regions within low- to intermediate-mass Why: protostellar clusters. Our observations include interferometer (i.e. CARMA) and single dish (e.g. FCRAO, IRAM 30m, APEX) To recover flux over a range of spatial scales in the region observations, probing scales over several orders of magnitude. How: Based on these observations, we calculate the masses and kinematics of outflows in these regions, and provide constraints for Jy beam km s Joint deconvolution method (Stanimirovic 2002), CARMA-only v=-2 to 6 km/s CARMA-only v=10 to 17 km/s models of clustered star formation. These results are presented for NGC 1333 by Plunkett et al. (2013, ApJ accepted), and -1 comparisons among star-forming regions at different evolutionary stages are forthcoming. using the analysis package MIRIAD. -1 1212COCO Example: We mapped NGC 1333 using CARMA with a resolution of ~5’’ (or 0.006 pc, 1000 AU) in order to Our study focuses on Class 0 & I outflow-driving protostars found in clusters, and we seek to detect outflows and associate them with their driving sources. understand their impact on the protocluster environment. To the right, we label several tracers CARMA+FCRAO v=-2 to 6 km/s CARMA+FCRAO v=10 to 17 km/s Jy beam km s 12 CONTINUUMCONTINUUM important to our study of cores (i.e. continuum), outflows ( CO) and their impact on the -1 13 The single dish FCRAO map of NGC 1333 is used envelope and cloud (13CO). Further, the temperature structure of these components is COCO -1 to recover the flux over larger spatial scales determined by observing several energy-level transitions of these molecules. (up to the map size of ~8’, or 0.5 pc) (Figure 5 of van Dishoeck et al. 2011) that is resolved out by the interferometer. 1212COCO Case Study: NGC 1333 Serpens South Plunkett et al. (2013, ApJ accepted) vout=-3 to -10 km/s vout=-10 to -30 km/s @ 415 pc 0.5 pc vout=-5 to -2 km/s vout=-8 to -5 km/s vout=-10 to -8 km/s = 3 to 10 km/s = 10 to 30 km/s = 1 to 3 km/s = 3 to 7 km/s = 7 to 9 km/s ows C3 C4 Region I: SVS 13 fl F4 ows fl SVS 13A SVS13A F1 Out + + B + C F3 F2 F3 Out Region II: IRAS 2 Background: IRAC 4.5 μm Red/Blue contours: CARMA CO(1-0) White contours: 2.7 mm continuum About + + +A + + + Spitzer IRAC Spitzer IRAC B Gutermuth et al. (2008a) APEX Location: Serpens; RA 18:30, dec -02:02 Gutermuth et al. (2008b) CO(3-2) Distance: 415 pc (Dzib et al. 2010) Age: ~2x105 yrs, very young “protocluster” (Gutermuth et al. 2008a) <CARMA mapped region> Membership: Protostar fraction (class I relative to all YSOs) of 80% at Region IV SK1 Western Knot Background: center (Nakamura et al. 2011) Region I IRAC 4.5 μm Contours: CARMA Significance: Protostars densely clustered along a central filamentary CO(1-0) SK 14 Region III: IRAS 4 -2 Region II structure, where high number density of protostars (reaching 430 pc at the center) likely has a profound impact on the cloud. + + 4D+ IRAS 4 + + + 4A + + + + 4C+ +4B C2 C1 C2 Circinus and M8 Region III Region IV: SVS 13C, SK 14 Region V 1 pc @ d=1250 pc ow fl About NGC 1333 Out Candidates Location: Perseus; RA 03:29, dec 31:14 + + Distance: 235 pc (Hirota et al. 2008) +SVS 13C 6 Age: ~10 years (Lada et al. 1996) SK 14 Members: 39 protostars, 98 pre-MS stars with disks, two late-B stars to north (Gutermuth et al. 2008b) APEX APEX WISE (22, 12, 4.6 micron) Spitzer IRAC CO(3-2) CO(3-2) Significance: NGC 1333 is considered the prototypical cluster, commonly used to model Liu et al. (2011) Credit: NASA/JPL-Caltech clustered star formation and outflow-driven turbulence (e.g. Nakamura & Li 2007). Circinus M8 (Lagoon) Location: 15h, -63° Location: Sag-Carina Arm; 18h, -24° NGC 1333 Results Distance: 700 pc (Bally et al. 1999) Distance: 1250 pc (Arias et al. 2006) Significance: Three IRAS point Significance: A more massive, more •Within NGC 1333, outflow kinetic energy, cloud gravitational energy and turbulent energy suggest that outflows act as an sources (marked to the right with evolved counter-part to the other red stars, Shimoikura & Dobashi regions in our survey, yet M8 important agent for turbulence in the region, and over time could disrupt the most active region of the cloud. 2011) are likely driving outflows in remains an active site of star the mapped region. It is apparent formation. Within the mapped •We identify outflows associated with 5 (of 7) Class 0 and 2 (of 4) Class I sources within the mapped region of NGC 1333. from the CO map that the red- region are many sub-mm gas shifted molecular outflow emission clumps (open stars) and Class 0/I is more dispersed than the blue. objects (yellow stars), based on •~10-25% of the final mass of a protostar comprises the protostellar wind and may drive momentum in the cluster environment, Kumar & Anandarao (2010). and should be taken into account in models that investigate the impact of outflows during early protostellar evolution. •Similar analyses of the regions Serpens South, Circinus and M8 are ongoing. How do the outflow References Arias, J.I., et al. 2006, MNRAS 366, 739 ● Bally, J., Reipurth, B., Lada, C. J., & Billawala, Y. 1999, AJ, 117, 410 ● Dzib, S., Loinard, L., Mioduszewski, A.J., et characteristics apparent in NGC 1333 evolve with, depend on, and/or affect their surrounding environments? al. 2010, ApJ, 718, 610 ● Gutermuth, R.A., Bourke, T.L., Allen, L.E., et al. 2008a, ApJL, 673, L151 ● Gutermuth, R. A., et al. 2008b, ApJ, 674, 336 ● Hirota, T., Bushimata, T., Choi, Y.K., et al. 2008, PASJ, 60, 37 ● Kumar, D. L., & Anandarao, B. G. 2010, MNRAS, 407, 1170 ● Lada, C.J., Alves, J., & Lada, E.A. 1996, AJ, 111, 1964 ● Nakamura, F., & •Preliminary analysis of Serpens South suggests that at least four sources are driving outflows from within a Li, Z.Y. 2007, ApJ, 662, 395 ● Nakamura, F., Sugitani, K., Shimajiri, Y., et al. 2011, ApJ, 737, 56 ● Shimoikura, T., & Dobashi, K. 2011, ApJ, 731, 23 ● Stanimirovic, S. 2002, Single-Dish Radio Astronomy: Techniques and Applications, 375–396 ● van Dishoeck, E.F., & Blake, G.A. 1998, ARA&A, 36, 317 ● van Dishoeck, E.F., Kristensen, L.E., region much more dense and active than the region we mapped in NGC 1333. Benz, A.O., et al. 2011, PASP, 123, 138 •Single-dish observations of Circinus and M8 provide evidence of outflow activity, and with higher-resolution Acknowledgements A.L.P. is a NSF Graduate Research Fellow. A.L.P. was supported by mosaic observations we will associate driving sources and molecular outflow emission across several parsecs. Fulbright Chile in 2012, and hosted at Cerro Calán, Universidad de Chile in 2012-13. This project is supported by the National Science Foundation under grant AST-0845619 made to H.G.A. •The extent to which we can identify outflows and their driving sources may correlate with the evolutionary Summary state of the cluster environment, and the possibility for outflows to disrupt the cloud over time..
Load more

Recommended publications
  • The Dunhuang Chinese Sky: a Comprehensive Study of the Oldest Known Star Atlas
    25/02/09JAHH/v4 1 THE DUNHUANG CHINESE SKY: A COMPREHENSIVE STUDY OF THE OLDEST KNOWN STAR ATLAS JEAN-MARC BONNET-BIDAUD Commissariat à l’Energie Atomique ,Centre de Saclay, F-91191 Gif-sur-Yvette, France E-mail: [email protected] FRANÇOISE PRADERIE Observatoire de Paris, 61 Avenue de l’Observatoire, F- 75014 Paris, France E-mail: [email protected] and SUSAN WHITFIELD The British Library, 96 Euston Road, London NW1 2DB, UK E-mail: [email protected] Abstract: This paper presents an analysis of the star atlas included in the medieval Chinese manuscript (Or.8210/S.3326), discovered in 1907 by the archaeologist Aurel Stein at the Silk Road town of Dunhuang and now held in the British Library. Although partially studied by a few Chinese scholars, it has never been fully displayed and discussed in the Western world. This set of sky maps (12 hour angle maps in quasi-cylindrical projection and a circumpolar map in azimuthal projection), displaying the full sky visible from the Northern hemisphere, is up to now the oldest complete preserved star atlas from any civilisation. It is also the first known pictorial representation of the quasi-totality of the Chinese constellations. This paper describes the history of the physical object – a roll of thin paper drawn with ink. We analyse the stellar content of each map (1339 stars, 257 asterisms) and the texts associated with the maps. We establish the precision with which the maps are drawn (1.5 to 4° for the brightest stars) and examine the type of projections used.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Arxiv:2005.05466V1 [Astro-Ph.GA] 11 May 2020 Surface Density
    Draft version May 13, 2020 Typeset using LATEX preprint style in AASTeX62 Star-Gas Surface Density Correlations in Twelve Nearby Molecular Clouds I: Data Collection and Star-Sampled Analysis Riwaj Pokhrel,1, 2 Robert A. Gutermuth,2 Sarah K. Betti,2 Stella S. R. Offner,3 Philip C. Myers,4 S. Thomas Megeath,1 Alyssa D. Sokol,2 Babar Ali,5 Lori Allen,6 Tom S. Allen,7, 8 Michael M. Dunham,9 William J. Fischer,10 Thomas Henning,11 Mark Heyer,2 Joseph L. Hora,4 Judith L. Pipher,12 John J. Tobin,13 and Scott J. Wolk4 1Ritter Astrophysical Research Center, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA 2Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003, USA 3Department of Astronomy, The University of Texas at Austin, 2500 Speedway, Austin, TX 78712, USA 4Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 5Space Sciences Institute, 4750 Walnut Street, Suite 205, Boulder, CO, USA 6National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ, 85719, USA 7Portland State University, 1825 SW Broadway Portland, OR 97207, USA 8Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA 9Department of Physics, State University of New York at Fredonia, 280 Central Ave, Fredonia, NY 14063, USA 10Space Telescope Science Institute, Baltimore, MD 21218, USA 11Max-Planck-Institute for Astronomy, K¨onigstuhl17, D-69117 Heidelberg, Germany 12Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA 13National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA (Received ...; Revised ...; Accepted May 13, 2020) Submitted to ApJ ABSTRACT We explore the relation between the stellar mass surface density and the mass surface density of molecular hydrogen gas in twelve nearby molecular clouds that are located at <1.5 kpc distance.
    [Show full text]
  • Scutum Apus Aquarius Aquila Ara Bootes Canes Venatici Capricornus Centaurus Cepheus Circinus Coma Berenices Corona Austrina Coro
    Polaris Ursa Minor Cepheus Camelopardus Thuban Draco Cassiopeia Mizar Ursa Major Lacerta Lynx Deneb Capella Perseus Auriga Canes Venatici Algol Cygnus Vega Cor Caroli Andromeda Lyra Bootes Leo Minor Castor Triangulum Corona Borealis Albireo Hercules Pollux Alphecca Gemini Vulpecula Coma Berenices Pleiades Aries Pegasus Sagitta Arcturus Taurus Cancer Aldebaran Denebola Leo Delphinus Serpens [Caput] Regulus Equuleus Altair Canis Minor Pisces Betelgeuse Aquila Procyon Orion Serpens [Cauda] Ophiuchus Virgo Sextans Monoceros Mira Scutum Rigel Aquarius Spica Cetus Libra Crater Capricornus Hydra Sirius Corvus Lepus Deneb Kaitos Canis Major Eridanus Antares Fomalhaut Piscis Austrinus Sagittarius Scorpius Antlia Pyxis Fornax Sculptor Microscopium Columba Caelum Corona Austrina Lupus Puppis Grus Centaurus Vela Norma Horologium Phoenix Telescopium Ara Canopus Indus Crux Pictor Achernar Hadar Carina Dorado Tucana Circinus Rigel Kentaurus Reticulum Pavo Triangulum Australe Musca Volans Hydrus Mensa Apus SampleOctans file Chamaeleon AND THE LONELY WAR Sample file STAR POWER VOLUME FOUR: STAR POWER and the LONELY WAR Copyright © 2018 Michael Terracciano and Garth Graham. All rights reserved. Star Power, the Star Power logo, and all characters, likenesses, and situations herein are trademarks of Michael Terracciano and Garth Graham. Except for review purposes, no portion of this publication may be reproduced or transmitted, in any form or by any means, without the express written consent of the copyright holders. All characters and events in this publication are fictional and any resemblance to real people or events is purely coincidental. Star chartsSample adapted from charts found at hoshifuru.jp file Portions of this book are published online at www.starpowercomic.com. This volume collects STAR POWER and the LONELY WAR Issues #16-20 published online between Oct 2016 and Oct 2017.
    [Show full text]
  • Educator's Guide: Orion
    Legends of the Night Sky Orion Educator’s Guide Grades K - 8 Written By: Dr. Phil Wymer, Ph.D. & Art Klinger Legends of the Night Sky: Orion Educator’s Guide Table of Contents Introduction………………………………………………………………....3 Constellations; General Overview……………………………………..4 Orion…………………………………………………………………………..22 Scorpius……………………………………………………………………….36 Canis Major…………………………………………………………………..45 Canis Minor…………………………………………………………………..52 Lesson Plans………………………………………………………………….56 Coloring Book…………………………………………………………………….….57 Hand Angles……………………………………………………………………….…64 Constellation Research..…………………………………………………….……71 When and Where to View Orion…………………………………….……..…77 Angles For Locating Orion..…………………………………………...……….78 Overhead Projector Punch Out of Orion……………………………………82 Where on Earth is: Thrace, Lemnos, and Crete?.............................83 Appendix………………………………………………………………………86 Copyright©2003, Audio Visual Imagineering, Inc. 2 Legends of the Night Sky: Orion Educator’s Guide Introduction It is our belief that “Legends of the Night sky: Orion” is the best multi-grade (K – 8), multi-disciplinary education package on the market today. It consists of a humorous 24-minute show and educator’s package. The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to alleviate the fear of space and the night sky (that many elementary and middle school teachers have) when it comes to that section of the science lesson plan. It is an excellent tool that allows the parents to be a part of the learning experience. The guide is devised in such a way that there are plenty of visuals to assist the educator and student in finding the Winter constellations.
    [Show full text]
  • Molecular Gas Conditions in NGC 4945 and the Circinus Galaxy?
    A&A 367, 457–469 (2001) Astronomy DOI: 10.1051/0004-6361:20000462 & c ESO 2001 Astrophysics Molecular gas conditions in NGC 4945 and the Circinus galaxy? S. J. Curran1,2,L.E.B.Johansson1,P.Bergman1, A. Heikkil¨a1,3, and S. Aalto1 1 Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden 2 European Southern Observatory, Casilla 19001, Santiago 19, Chile 3 Observatory, PO Box 14, 00014 University of Helsinki, Finland Received 11 July 2000 / Accepted 5 December 2000 Abstract. We present results of a multi-transition study of the dense molecular gas in the central part of the hybrid star-burst/Seyfert galaxies NGC 4945 and the Circinus galaxy. From the results of radiative transfer 3− 4 −3 ≈ calculations, we estimate in NGC 4945 nH2 =310 10 cm and Tkin 100 K and in Circinus nH2 = 3 5 −3 210−10 cm and Tkin ≈ 50−80 K for the molecular hydrogen density and kinetic temperature, respectively. As well as density/temperature tracing molecules, we have observed C17OandC18O in each galaxy and the value of C18O/C17O ≈ 6 for the isotopic column density ratio suggests that both have relatively high populations of massive stars. Finally, although star formation is present, the radiative transfer results combined with the high HCN/CO and (possibly) HCN/FIR, radio/FIR ratios may suggest that, in comparison with Circinus, a higher proportion of the dense gas emission in NGC 4945 may be located in the hypothesised central nuclear disk as opposed to dense star forming cloud cores. Contrary to the literature, which assumes that all of the far-infrared emission arises from star formation, our results suggest that in NGC 4945 some of this emission could arise from an additional source, and so we believe that a revision of the star formation rate estimates may be required for these two galaxies.
    [Show full text]
  • Sydney Observatory Night Sky Map September 2012 a Map for Each Month of the Year, to Help You Learn About the Night Sky
    Sydney Observatory night sky map September 2012 A map for each month of the year, to help you learn about the night sky www.sydneyobservatory.com This star chart shows the stars and constellations visible in the night sky for Sydney, Melbourne, Brisbane, Canberra, Hobart, Adelaide and Perth for September 2012 at about 7:30 pm (local standard time). For Darwin and similar locations the chart will still apply, but some stars will be lost off the southern edge while extra stars will be visible to the north. Stars down to a brightness or magnitude limit of 4.5 are shown. To use this chart, rotate it so that the direction you are facing (north, south, east or west) is shown at the bottom. The centre of the chart represents the point directly above your head, called the zenith, and the outer circular edge represents the horizon. h t r No Star brightness Moon phase Last quarter: 08th Zero or brighter New Moon: 16th 1st magnitude LACERTA nd Deneb First quarter: 23rd 2 CYGNUS Full Moon: 30th rd N 3 E LYRA th Vega W 4 LYRA N CORONA BOREALIS HERCULES BOOTES VULPECULA SAGITTA PEGASUS DELPHINUS Arcturus Altair EQUULEUS SERPENS AQUILA OPHIUCHUS SCUTUM PISCES Moon on 23rd SERPENS Zubeneschamali AQUARIUS CAPRICORNUS E SAGITTARIUS LIBRA a Saturn Centre of the Galaxy Antares Zubenelgenubi t s Antares VIRGO s t SAGITTARIUS P SCORPIUS P e PISCESMICROSCOPIUM AUSTRINUS SCORPIUS Mars Spica W PISCIS AUSTRINUS CORONA AUSTRALIS Fomalhaut Centre of the Galaxy TELESCOPIUM LUPUS ARA GRUSGRUS INDUS NORMA CORVUS INDUS CETUS SCULPTOR PAVO CIRCINUS CENTAURUS TRIANGULUM
    [Show full text]
  • Arxiv:2004.14050V1 [Astro-Ph.SR] 29 Apr 2020
    Draft version April 30, 2020 Typeset using LATEX twocolumn style in AASTeX63 A detailed analysis on the cloud structure and dynamics in Aquila Rift Tomomi Shimoikura,1 Kazuhito Dobashi,2 Yoshiko Hatano,2 and Fumitaka Nakamura3, 4 1Otsuma Women's University ` Chiyoda-ku,Tokyo, 102-8357, Japan 2Tokyo Gakugei University Koganei, 184-8501, Tokyo 3National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan 4Department of Astronomical Science, School of Physical Science, SOKENDAI (The Graduate University for Advanced Studies), Osawa, Mitaka, Tokyo 181-8588, Japan (Accepted April 23, 2020) Submitted to APJ ABSTRACT We present maps in several molecular emission lines of a 1 square-degree region covering the W40 and Serpens South molecular clouds belonging to the Aquila Rift complex. The observations were made with the 45 m telescope at the Nobeyama Radio Observatory. We found that the 12CO and 13CO emission lines consist of several velocity components with different spatial distributions. The component that forms the main cloud of W40 and Serpens South, which we call the \main component", −1 −1 has a velocity of VLSR ' 7 km s . There is another significant component at VLSR ' 40 km s , which we call the \40 km s−1 component". The latter component is mainly distributed around two young clusters: W40 and Serpens South. Moreover, the two components look spatially anti-correlated. Such spatial configuration suggests that the star formation in W40 and Serpens South was induced by the collision of the two components. We also discuss a possibility that the 40 km s−1 component consists of gas swept up by superbubbles created by SNRs and stellar winds from the Scorpius-Centaurus Association.
    [Show full text]
  • These Sky Maps Were Made Using the Freeware UNIX Program "Starchart", from Alan Paeth and Craig Counterman, with Some Postprocessing by Stuart Levy
    These sky maps were made using the freeware UNIX program "starchart", from Alan Paeth and Craig Counterman, with some postprocessing by Stuart Levy. You’re free to use them however you wish. There are five equatorial maps: three covering the equatorial strip from declination −60 to +60 degrees, corresponding roughly to the evening sky in northern winter (eq1), spring (eq2), and summer/autumn (eq3), plus maps covering the north and south polar areas to declination about +/− 25 degrees. Grid lines are drawn at every 15 degrees of declination, and every hour (= 15 degrees at the equator) of right ascension. The equatorial−strip maps use a simple rectangular projection; this shows constellations near the equator with their true shape, but those at declination +/− 30 degrees are stretched horizontally by about 15%, and those at the extreme 60−degree edge are plotted twice as wide as you’ll see them on the sky. The sinusoidal curve spanning the equatorial strip is, of course, the Ecliptic −− the path of the Sun (and approximately that of the planets) through the sky. The polar maps are plotted with stereographic projection. This preserves shapes of small constellations, but enlarges them as they get farther from the pole; at declination 45 degrees they’re about 17% oversized, and at the extreme 25−degree edge about 40% too large. These charts plot stars down to magnitude 5, along with a few of the brighter deep−sky objects −− mostly star clusters and nebulae. Many stars are labelled with their Bayer Greek−letter names. Also here are similarly−plotted maps, based on galactic coordinates.
    [Show full text]
  • Special Spitzer Telescope Edition No
    INFRARED SCIENCE INTEREST GROUP Special Spitzer Telescope Edition No. 4 | August 2020 Contents From the IR SIG Leadership Council In the time since our last newsletter in January, the world has changed. 1 From the SIG Leadership Travel restrictions and quarantine have necessitated online-conferences, web-based meetings, and working from home. Upturned semesters, constantly shifting deadlines and schedules, and the evolving challenge of Science Highlights keeping our families and communities safe have all taken their toll. We hope this newsletter offers a moment of respite and a reminder that our community 2 Mysteries of Exoplanet continues its work even in the face of great uncertainty and upheaval. Atmospheres In January we said goodbye to the Spitzer Space Telescope, which 4 Relevance of Spitzer in the completed its mission after sixteen years in space. In celebration of Spitzer, Era of Roman, Euclid, and in recognition of the work of so many members of our community, this Rubin & SPHEREx newsletter edition specifically highlights cutting edge science based on and inspired by Spitzer. In the words of Dr. Paul Hertz, Director of Astrophysics 6 Spitzer: The Star-Formation at NASA: Legacy Lives On "Spitzer taught us how important infrared light is to our 8 AKARI Spitzer Survey understanding of our universe, both in our own cosmic 10 Science Impact of SOFIA- neighborhood and as far away as the most distant galaxies. HIRMES Termination The advances we make across many areas in astrophysics in the future will be because of Spitzer's extraordinary legacy." Technical Highlights Though Spitzer is gone, our community remains optimistic and looks forward to the advances that the next generation of IR telescopes will bring.
    [Show full text]
  • A Compendium of Distances to Molecular Clouds in the Star Formation Handbook?,?? Catherine Zucker1, Joshua S
    A&A 633, A51 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936145 & c ESO 2020 Astrophysics A compendium of distances to molecular clouds in the Star Formation Handbook?,?? Catherine Zucker1, Joshua S. Speagle1, Edward F. Schlafly2, Gregory M. Green3, Douglas P. Finkbeiner1, Alyssa Goodman1,5, and João Alves4,5 1 Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA e-mail: [email protected], [email protected] 2 Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA 3 Kavli Institute for Particle Astrophysics and Cosmology, Physics and Astrophysics Building, 452 Lomita Mall, Stanford, CA 94305, USA 4 University of Vienna, Department of Astrophysics, Türkenschanzstraße 17, 1180 Vienna, Austria 5 Radcliffe Institute for Advanced Study, Harvard University, 10 Garden St, Cambridge, MA 02138, USA Received 21 June 2019 / Accepted 12 August 2019 ABSTRACT Accurate distances to local molecular clouds are critical for understanding the star and planet formation process, yet distance mea- surements are often obtained inhomogeneously on a cloud-by-cloud basis. We have recently developed a method that combines stellar photometric data with Gaia DR2 parallax measurements in a Bayesian framework to infer the distances of nearby dust clouds to a typical accuracy of ∼5%. After refining the technique to target lower latitudes and incorporating deep optical data from DECam in the southern Galactic plane, we have derived a catalog of distances to molecular clouds in Reipurth (2008, Star Formation Handbook, Vols. I and II) which contains a large fraction of the molecular material in the solar neighborhood. Comparison with distances derived from maser parallax measurements towards the same clouds shows our method produces consistent distances with .10% scatter for clouds across our entire distance spectrum (150 pc−2.5 kpc).
    [Show full text]
  • Molecular Jets and Outflows from Young Stellar Objects in Cygnus-X, Auriga, and Cassiopeia
    Kent Academic Repository Full text document (pdf) Citation for published version Makin, Sally Victoria (2019) Molecular jets and outflows from young stellar objects in Cygnus-X, Auriga, and Cassiopeia. Doctor of Philosophy (PhD) thesis, University of Kent,. DOI Link to record in KAR https://kar.kent.ac.uk/72857/ Document Version UNSPECIFIED Copyright & reuse Content in the Kent Academic Repository is made available for research purposes. Unless otherwise stated all content is protected by copyright and in the absence of an open licence (eg Creative Commons), permissions for further reuse of content should be sought from the publisher, author or other copyright holder. Versions of research The version in the Kent Academic Repository may differ from the final published version. Users are advised to check http://kar.kent.ac.uk for the status of the paper. Users should always cite the published version of record. Enquiries For any further enquiries regarding the licence status of this document, please contact: [email protected] If you believe this document infringes copyright then please contact the KAR admin team with the take-down information provided at http://kar.kent.ac.uk/contact.html UNIVERSITY OF KENT DOCTORAL THESIS Molecular jets and outflows from young stellar objects in Cygnus-X, Auriga, and Cassiopeia Author: Supervisor: Sally Victoria MAKIN Dr. Dirk FROEBRICH A thesis submitted in fulfilment of the requirements for the degree of Doctor of Philosophy in the Centre for Astrophysics and Planetary Science School of Physical Sciences January 30, 2019 Declaration of Authorship I, Sally Victoria MAKIN, declare that this thesis titled, “Molecular jets and outflows from young stellar objects in Cygnus-X, Auriga, and Cassiopeia” and the work presented in it are my own.
    [Show full text]