Precision Single Mode Fibre Integral Field Spectroscopy with the RHEA Spectrograph
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I. Deep Search for N2H+ in the Protoplanetary Disks Around Lkca
A&A 464, 615–623 (2007) Astronomy DOI: 10.1051/0004-6361:20065385 & c ESO 2007 Astrophysics Chemistry in disks + I. Deep search for N2H in the protoplanetary disks around LkCa 15, MWC 480, and DM Tauri A. Dutrey1, T. Henning2, S. Guilloteau1,D.Semenov2,V.Piétu3,K.Schreyer4, A. Bacmann1, R. Launhardt2, J. Pety3,andF.Gueth3 1 L3AB, Observatoire de Bordeaux, 2 rue de l’Observatoire, BP 89, 33270 Floirac, France e-mail: [email protected] 2 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 3 IRAM, 300 rue de la Piscine, 38406 Saint-Martin-d’Hères, France 4 Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergässchen 2-3, 07745 Jena, Germany Received 7 April 2006 / Accepted 21 November 2006 ABSTRACT Aims. To constrain the ionization fraction in protoplanetary disks, we present new high-sensitivity interferometric observations + of N2H in three disks surrounding DM Tau, LkCa 15, and MWC 480. + 2 Methods. We used the IRAM PdBI array to observe the N2H J = 1−0 line and applied a χ -minimization technique to estimate corresponding column densities. These values are compared, together with HCO+ column densities, to results of a steady-state disk model with a vertical temperature gradient coupled to gas-grain chemistry. + Results. We report two N2H detections for LkCa 15 and DM Tau at the 5σ level and an upper limit for MWC 480. The column den- + + sity derived from the data for LkCa 15 is much lower than previously reported. The [N2H /HCO ] ratio is on the order of 0.02−0.03. -
Hot Gas Lines in T Tauri Stars
Smith ScholarWorks Astronomy: Faculty Publications Astronomy 7-2013 Hot Gas Lines in T Tauri Stars David R. Ardila California Institute of Technology Gregory J. Herczeg Peking University Scott G. Gregory California Institute of Technology Laura Ingleby University of Michigan Kevin France University of Colorado, Boulder See next page for additional authors Follow this and additional works at: https://scholarworks.smith.edu/ast_facpubs Part of the Astrophysics and Astronomy Commons Recommended Citation Ardila, David R.; Herczeg, Gregory J.; Gregory, Scott G.; Ingleby, Laura; France, Kevin; Brown, Alexander; Edwards, Suzan; Johns-Krull, Christopher; Linsky, Jeffrey L.; Yang, Hao; Valenti, Jeff A.; Abgrall, Hervé; Alexander, Richard D.; Bergin, Edwin; Bethell, Thomas; Brown, Joanna M.; Calvet, Nuria; Espaillat, Catherine; Hillenbrand, Lynne A.; Hussain, Gaitee; Roueff, Evelyne; Schindhelm, Eric R.; and Walter, Frederick M., "Hot Gas Lines in T Tauri Stars" (2013). Astronomy: Faculty Publications, Smith College, Northampton, MA. https://scholarworks.smith.edu/ast_facpubs/23 This Article has been accepted for inclusion in Astronomy: Faculty Publications by an authorized administrator of Smith ScholarWorks. For more information, please contact [email protected] Authors David R. Ardila, Gregory J. Herczeg, Scott G. Gregory, Laura Ingleby, Kevin France, Alexander Brown, Suzan Edwards, Christopher Johns-Krull, Jeffrey L. Linsky, Hao Yang, Jeff A. Valenti, Hervé Abgrall, Richard D. Alexander, Edwin Bergin, Thomas Bethell, Joanna M. Brown, Nuria Calvet, Catherine Espaillat, Lynne A. Hillenbrand, Gaitee Hussain, Evelyne Roueff, Eric R. Schindhelm, and Frederick M. Walter This article is available at Smith ScholarWorks: https://scholarworks.smith.edu/ast_facpubs/23 The Astrophysical Journal Supplement Series, 207:1 (43pp), 2013 July doi:10.1088/0067-0049/207/1/1 C 2013. -
THE AGB NEWSLETTER an Electronic Publication Dedicated to Asymptotic Giant Branch Stars and Related Phenomena
THE AGB NEWSLETTER An electronic publication dedicated to Asymptotic Giant Branch stars and related phenomena No. 117 | 1 February 2007 http://www.astro.keele.ac.uk/AGBnews Editors: Jacco van Loon and Albert Zijlstra Editorial Dear Colleagues, It is our pleasure to present you the 117th issue of the AGB Newsletter. Of the 21 refereed journal publications, eight deal directly with Planetary Nebulae | which may have something to do with planets after all, and perhaps with dark energy as well (see the contribution by Gibson & Schild). Don't miss the many job advertisements, both for PhD studentships (Denver, Vienna, Portsmouth) and postdoctoral fellowships (Vienna, Keele). The Food for Thought statement published last month generated some reaction. One of you considered the relation between rotation rate and magnetic activity to be the principal question in relation to AGB stars that needs to be answered. Hence, we make it this month's Food for Thought statement. Reactions to this, or suggestions for other pertinent questions, are very welcome and will be discussed in future issues of the newsletter. The next issue will be distributed on the 1st of March; the deadline for contributions is the 28th of February. Editorially Yours, Jacco van Loon and Albert Zijlstra Food for Thought This month's thought-provoking statement is: The relation between rotation rate and magnetic activity is the principal question in relation to AGB stars that needs to be answered Reactions to this statement or suggestions for next month's statement can be e-mailed to [email protected] (please state whether you wish to remain anonymous) 1 Refereed Journal Papers Magnetic ¯elds in planetary nebulae and post-AGB nebulae. -
Arxiv:0805.2293V1 [Astro-Ph] 15 May 2008 Iemaueet F(U)Ilmtreiso Rmc (Aft CO from Emission H (Sub)Millimeter of Sens Complementary, Measurements 2001)
Astronomy & Astrophysics manuscript no. 9742ms c ESO 2008 May 16, 2008 Molecules in the Circumstellar Disk Orbiting BP Piscium Research Note Joel H. Kastner1,2, B. Zuckerman3,4, and Thierry Forveille1 1 Laboratoire d’Astrophysique de Grenoble, Universit´eJoseph Fourier — CNRS, BP 53, 38041 Grenoble Cedex, France e-mail: [email protected] 2 Chester F. Carlson Center for Imaging Science, Rochester Institute of Technology, 54 Lomb Memorial Dr., Rochester, NY 14623 USA 3 Dept. of Physics & Astronomy, University of California, Los Angeles 90095 USA 4 UCLA Center for Astrobiology, University of California, Los Angeles 90095 USA Received ...; accepted ... ABSTRACT Context. BP Psc is a puzzling late-type, emission-line field star with large infrared excess. The star is encircled and enshrouded by a nearly edge-on, dusty circumstellar disk, and displays an extensive jet system similar to those associated with pre-main sequence (pre-MS) stars. However, the photospheric absorption features of the star itself appear more consistent with post-main sequence status. Aims. We seek to characterize the molecular gas component of the BP Psc disk, so as to compare the properties of its molecular disk with those of well-studied pre-main sequence stars. Methods. We conducted a mm-wave molecular line survey of BP Psc with the 30 m telescope of the Institut de Radio Astronomie Millimetrique (IRAM). We use these data to investigate the kinematics, gas mass, and chemical constituents of the BP Psc disk. 12 13 + Results. We detected lines of CO and CO and, possibly, very weak emission from HCO and CN; HCN, H2CO, and SiO are not detected. -
The Architecture of the Lkca 15 Transitional Disk Revealed by High-Contrast Imaging
UvA-DARE (Digital Academic Repository) The architecture of the LkCa 15 transitional disk revealed by high-contrast imaging Thalmann, C.; Mulders, G.D.; Hodapp, K.; Janson, M.; Grady, C.A.; Min, M.; de Juan Ovelar, M.; Carson, J.; Brandt, T.; Bonnefoy, M.; McElwain, M.W.; Leisenring, J.; Dominik, C.; Henning, T.; Tamura, M. DOI 10.1051/0004-6361/201322915 Publication date 2014 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Thalmann, C., Mulders, G. D., Hodapp, K., Janson, M., Grady, C. A., Min, M., de Juan Ovelar, M., Carson, J., Brandt, T., Bonnefoy, M., McElwain, M. W., Leisenring, J., Dominik, C., Henning, T., & Tamura, M. (2014). The architecture of the LkCa 15 transitional disk revealed by high-contrast imaging. Astronomy & Astrophysics, 566, A51. https://doi.org/10.1051/0004- 6361/201322915 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. -
Optical Spectroscopy of Embedded Young Stars in the Taurus-Auriga Molecular Cloud
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Optical Spectroscopy of Embedded Young Stars in the Taurus-Auriga Molecular Cloud Scott J. Kenyon Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 e-mail: [email protected] David I. Brown Jet Propulsion Laboratory, MS 156-205, 4800 Oak Grove Drive, Pasadena, CA 91109 e-mail: [email protected] Christopher A. Tout Institute of Astronomy, Madingley Road, Cambridge CB3 0HA England e-mail: [email protected] and Perry Berlind Whipple Observatory, PO Box 97, Amado, AZ 85645 e-mail: [email protected] to appear in The Astronomical Journal June 1998 –2– ABSTRACT This paper describes the first optical spectroscopic survey of class I sources (also known as embedded sources and protostars) in the Taurus-Auriga dark cloud. We detect 10 of the 24 known class I sources in the cloud at 5500–9000 A.˚ All detected class I sources have strong Hα emission; most also have strong [O I] and [S II] emission. These data – together with high quality optical spectra of T Tauri stars in the Taurus-Auriga cloud – demonstrate that forbidden emission lines are stronger and more common in class I sources than in T Tauri stars. Our results also provide a clear discriminant in the frequency of forbidden line emission between weak-emission and classical T Tauri stars. In addition to strong emission lines, three class I sources have prominent TiO absorption bands. The M-type central stars of these sources mingle with optically visible T Tauri stars in the HR diagram and lie somewhat below both the birthline for spherical accretion and the deuterium burning sequence for disc accretion. -
School of Physics Publications 2007
School of Physics Publications 2007 Books Karnutsch, C 2007, Low threshold organic thin-film laser devices, Göttingen, 1 Ostrikov, K, Xu, S 2007, Plasma-Aided Nanofabrication: From Plasma Sources to Nanoassembly, Weinheim, Germany Book Chapters Beck, R, Gaensler, B M, Feretti, L 2007, SKA and the Magnetic Universe, Exploring the Cosmic Frontier: Astrophysical Instruments for the 21st Century, Springer-Verlag Berlin Heidelberg, Berlin Heidelberg, 103-108 Bilek, M, Powles, R C, McKenzie, D R 2007, Treatment of polymeric biomaterials by ion implantation, Biomaterials and Surface Modification, Research Signpost, India, 205-248 Britton, S C, New, P B, Roberts, A L, Sharma, M D 2007, Investigating students' ability totransfer mathematics, Transforming a university: the scholarship of teaching and learning in practice, University of Sydney Press, NSW, Australia, 127-140 Dey, C J, Berger, C, Foran, B, Foran, M, Joske, R, Lenzen, M, Wood, R J 2007, Household environmental pressure from consumption: an Australian environmental atlas, Water Wind Art and Debate -How environmental concerns impacton disciplinary research, Sydney University Press, Sydney, 1, 280-314 Eggleton, B J, Slusher, R 2007, Nonlinear pulse propagation in one-dimensional photonic bandgap structures, Nonlinear photonic bandgap materials, Springer Khoukhi, M, Maruyama, S, Bosi, S G, Komiya, A 2007, A Simple Approach for Calculating the Optical Constants of a Clear Glass Window from 0.19 to 5 um, Recent Developments in Solar Energy, Nova Science Publishers, Inc, New York, 289-297 -
X-Ray Emission of Multiple T Tauri Stars in Taurus
A&A 369, 971–980 (2001) Astronomy DOI: 10.1051/0004-6361:20010173 & c ESO 2001 Astrophysics X-ray emission of multiple T Tauri stars in Taurus B. K¨onig1, R. Neuh¨auser1;2, and B. Stelzer1 1 MPI f¨ur extraterrestrische Physik, Giessenbachstraße 1, 85740 Garching, Germany 2 Institute for Astronomy, University of Hawaii, Honolulu, USA Received 29 February 2000 / Accepted 26 January 2001 Abstract. We present a study of X-ray emission of known multiple T Tauri stars (TTS) in Taurus based on ROSAT observations. We used the ROSAT All-Sky Survey (RASS) detection rates of single classical (cTTS) and weak-line TTS (wTTS) to investigate statistically the TTS nature (classical or weak-line) of the components in multiple TTS, which are too close for spatially resolved spectroscopy so far. Because single wTTS show a higher RASS detection rate than single cTTS, the different binary TTS (cTTS-cTTS, cTTS-wTTS, wTTS-wTTS) should also have different detection rates. We find that the observed RASS detection rates of binary wTTS, where the nature of the secondary is unknown, are in agreement with the secondaries being wTTS rather than cTTS, and mixed pairs are very rare. Furthermore we analyse the X-ray emission of TTS systems resolvable by the ROSAT HRI. Among those systems we find statistical evidence that primaries show larger X-ray luminosity than secondaries, and that the samples of primary and secondary TTS are similar concerning the X-ray over bolometric luminosity ratios. Furthermore, primaries always emit harder X-rays than secondaries. In all cases where rotational velocities and/or periods are known for both companions, it is always the primary that rotates faster. -
Astrophysical Distance Scale II. Application of the JAGB Method: a Nearby Galaxy Sample Wendy L
Draft version May 22, 2020 Typeset using LATEX preprint style in AASTeX62 Astrophysical Distance Scale II. Application of the JAGB Method: A Nearby Galaxy Sample Wendy L. Freedman1 and Barry F. Madore1, 2 1Dept. of Astronomy & Astrophysics University of Chicago 5640 S. Ellis Ave., Chicago, IL, 60637 2The Observatories Carnegie Institution for Science 813 Santa Barbara St., Pasadena, CA 91101 ABSTRACT We apply the near-infrared J-region Asymptotic Giant Branch (JAGB) method, re- cently introduced by Madore & Freedman (2020), to measure the distances to 14 nearby galaxies out to 4 Mpc. We use the geometric detached eclipsing binary (DEB) distances to the LMC and SMC as independent zero-point calibrators. We find excellent agree- ment with previously published distances based on the Tip of the Red Giant Branch (TRGB): the JAGB distance determinations (including the LMC and SMC) agree in the mean to within ∆(JAGB T RGB) =+0.025 0.013 mag, just over 1%, where the − ± TRGB I-band zero point is MI = -4.05 mag. With further development and testing, the JAGB method has the potential to provide an independent calibration of Type Ia supernovae (SNe Ia), especially with JW ST . The JAGB stars (with M = 6:20 mag) J − can be detected farther than the fainter TRGB stars, allowing greater numbers of cal- ibrating galaxies for the determination of H0. Along with the TRGB and Cepheids, arXiv:2005.10793v1 [astro-ph.GA] 21 May 2020 JAGB stars are amenable to theoretical understanding and further refined empirical calibration. A preliminary test shows little dependence, if any, of the JAGB magnitude with metallicity of the parent galaxy. -
Magao-X: Project Status and First Laboratory Results
MagAO-X: project status and first laboratory results Jared R. Malesa, Laird M. Closea, Kelsey Millera,b, Lauren Schatza,b, David Doelmanc, Jennifer Lumbresa,b, Frans Snikc, Alex Rodacka,b, Justin Knighta,b, Kyle Van Gorkoma,b, Joseph D. Longa, Alex Hedglena,b, Maggie Kautza,b, Nemanja Jovanovicd, Katie Morzinskia, Olivier Guyona,b,e,f, Ewan Douglasg, Katherine B. Folletteh, Julien Lozie, Chris Bohlmana, Olivier Durneya, Victor Gashoa, Phil Hinza, Michael Irelandi, Madison Jeana,b, Christoph Kellerc, Matt Kenworthyc, Ben Mazinj, Jamison Noenickxa, Dan Alfreda, Kevin Pereza, Anna Sancheza, Corwynn Sauvea, Alycia Weinbergerk, and Al Conradl aSteward Observatory, University of Arizona bCollege of Optical Sciences, University of Arizona cSterrewacht Leiden, Universiteit Leiden dCaltech Optical Observatory, California Institute of Technology eSubaru Telescope, National Astronomical Observatory of Japan fAstrobiology Center, National Institutes of Natural Sciences, Japan gMassachusetts Institute of Technology, Department of Aeronautics and Astronautics hPhysics and Astronomy Department, Amherst College iThe Australian National University jDepartment of Physics, University of California Santa Barbara kDepartment of Terrestrial Magnetism, Carnegie Institution for Science lLarge Binocular Telescope Observatory ABSTRACT MagAO-X is an entirely new extreme adaptive optics system for the Magellan Clay 6.5 m telescope, funded by the NSF MRI program starting in Sep 2016. The key science goal of MagAO-X is high-contrast imaging of accreting protoplanets at Hα. With 2040 actuators operating at up to 3630 Hz, MagAO-X will deliver high Strehls (> 70%), high resolution (19 mas), and high contrast (< 1 × 10−4) at Hα (656 nm). We present an overview of the MagAO-X system, review the system design, and discuss the current project status. -
Born-Again Protoplanetary Disk Around Mira B M
The Astrophysical Journal, 662:651Y657, 2007 June 10 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. BORN-AGAIN PROTOPLANETARY DISK AROUND MIRA B M. J. Ireland Planetary Science, California Institute of Technology, Pasadena, CA 91125; [email protected] J. D. Monnier University of Michigan, Ann Arbor, MI 48109; [email protected] P. G. Tuthill School of Physics, University of Sydney, NSW 2006, Australia; [email protected] R. W. Cohen W. M. Keck Observatory, Kamuela, HI 96743 J. M. De Buizer Gemini Observatory, Casilla 603, La Serena, Chile C. Packham University of Florida, Gainsville, FL 32611 D. Ciardi Michelson Science Center, Caltech, Pasadena CA 91125 T. Hayward Gemini Observatory, Casilla 603, La Serena, Chile and J. P. Lloyd Cornell University, Ithaca, NY 14853 Received 2007 February 16; accepted 2007 March 10 ABSTRACT The Mira AB system is a nearby (107 pc) example of a wind accreting binary star system. In this class of system, the wind from a mass-losing red giant star (Mira A) is accreted onto a companion (Mira B), as indicated by an accretion shock signature in spectra at ultraviolet and X-ray wavelengths. Using novel imaging techniques, we report the detection of emission at mid-infrared wavelengths between 9.7 and 18.3 m from the vicinity of Mira B but with a peak at a radial position about 10 AU closer to the primary Mira A. We interpret the mid-infrared emission as the edge of an optically-thick accretion disk heated by Mira A. The discovery of this new class of accretion disk fed by M-giant mass loss implies a potential population of young planetary systems in white dwarf binaries, which has been little explored despite being relatively common in the solar neighborhood. -
Masses and Implications for Ages of Low-Mass Pre-Main Sequence Stars in Taurus and Ophiuchus
Draft version August 28, 2019 Preprint typeset using LATEX style AASTeX6 v. 1.0 MASSES AND IMPLICATIONS FOR AGES OF LOW-MASS PRE-MAIN SEQUENCE STARS IN TAURUS AND OPHIUCHUS M. Simon1,2, S. Guilloteau3, Tracy L. Beck4, E. Chapillon3,7, E. Di Folco3, A. Dutrey3, Gregory A. Feiden5 N. Grosso6,V. Pietu´ 7. L. Prato8, Gail H. Schaefer9 1Dept. of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA; [email protected] 2Dept. of Astrophysics, American Museum of Natural History, New York, NY 10024, USA 3Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, all´eeGeoffroy Saint-Hilaire, 33615 Pessac, France 4Space Telescope Science Institute, 3700 San Mateo Drive, Baltimore, MD 20218, USA 5Dept. of Physics and Astronomy, University of North Georgia, Dahlonega, GA, 30597, USA 6Aix Marseille University, CNRS, CNES, LAM, Marseille, France 7IRAM, 300 rue de la piscine, F-38406 Saint Martin d'H`eres,France 8Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA 9The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, CA 91023, USA ABSTRACT The accuracy of masses of pre-main sequence (PMS) stars derived from their locations on the Hertzsprung-Russell Diagram (HRD) can be tested by comparison with accurate and precise masses determined independently. We present 29 single stars in the Taurus star-forming region (SFR) and 3 in the Ophiuchus SFR with masses measured dynamically to a precision of at least 10%. Our results include 9 updated mass determinations and 3 that have not had their dynamical masses published before. This list of stars with fundamental, dynamical masses, Mdyn, is drawn from a larger list of 39 targets in the Taurus SFR and 6 in the Ophiuchus SFR.