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4 results on '"GALAXY EVOLUTION SAGE"'

1. The Polycyclic Aromatic Hydrocarbon Mass Fraction on a 10 pc Scale in the Magellanic Clouds

Author

Karl D. Gordon, Caroline Bot, Jérémy Chastenet, Yasuo Fukui, Adam K. Leroy, Dyas Utomo, Kisetsu Tsuge, Karin Sandstrom, I-Da Chiang, B. T. Draine, and Toshikazu Onishi

Subjects
010504 meteorology & atmospheric sciences, Milky Way, Metallicity, FOS: Physical sciences, Polycyclic aromatic hydrocarbon, Astrophysics, 01 natural sciences, SPITZER LEGACY PROGRAM, INFRARED-EMISSION BANDS, WARM IONIZED MEDIUM, PHOTOMETRIC SURVEY, 0103 physical sciences, Magellanic Clouds, GALAXY EVOLUTION SAGE, polycyclic compounds, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Cosmic dust, abundances [ISM], POINT-SOURCE CLASSIFICATION, Physics, chemistry.chemical_classification, extinction, Radiation field, Astronomy and Astrophysics, Plasma, Astrophysics - Astrophysics of Galaxies, Galaxy, Chemistry, Physics and Astronomy, chemistry, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MILKY-WAY, dust, MU-M PAH, Mass fraction, LOW-METALLICITY ENVIRONMENTS, INTERSTELLAR DUST
Abstract

We present maps of the dust properties in the Small and Large Magellanic Clouds (SMC, LMC) from fitting Spitzer and Herschel observations with the \citet{DL07} dust model. We derive the abundance of the small carbonaceous grain (or polycyclic aromatic hydrocarbon; PAH) component. The global PAH fraction (q_pah, the fraction of the dust mass in the form of PAHs) is smaller in the SMC (1.0$^{+0.3}_{-0.3}$%) than in the LMC (3.3$^{+1.4}_{-1.3}$%). We measure the PAH fraction in different gas phases (H II regions, ionized gas outside of H II regions, molecular gas, and diffuse neutral gas). H II regions appear as distinctive holes in the spatial distribution of the PAH fraction. In both galaxies, the PAH fraction in the diffuse neutral medium is higher than in the ionized gas, but similar to the molecular gas. Even at equal radiation field intensity, the PAH fraction is lower in the ionized gas than in the diffuse neutral gas. We investigate the PAH life-cycle as a function of metallicity between the two galaxies. The PAH fraction in the diffuse neutral medium of the LMC is similar to that of the Milky Way ($\sim4.6$%), while it is significantly lower in the SMC. Plausible explanations for the higher PAH fraction in the diffuse neutral medium of the LMC compared to the SMC include: a more effective PAH production by fragmentation of large grains at higher metallicity, and/or the growth of PAHs in molecular gas., Comment: Accepted for publication in ApJ

Published
2019

2. Hubble Tarantula Treasury Project. III. Photometric Catalog and Resulting Constraints on the Progression of Star Formation in the 30 Doradus Region

Author

Linda J. Smith, Dennis Zaritsky, Martha L. Boyer, J. E. Ryon, Karl D. Gordon, Eva K. Grebel, D. J. Lennon, J.S. Gallager, R. P. van der Marel, Dimitrios A. Gouliermis, H. Arab, G. De Marchi, Alessandra Aloisi, Anton M. Koekemoer, Peter Zeidler, James A. Anderson, Monica Tosi, S. E. de Mink, Elena Sabbi, Hugues Sana, Nino Panagia, Chris Evans, Michele Cignoni, S. S. Larsen, and Low Energy Astrophysics (API, FNWI)

Subjects
INITIAL MASS FUNCTION, Astronomy, Astrophysics, 01 natural sciences, Advanced Camera for Surveys, galaxies: star clusters: individual (30 Doradus), Magellanic Clouds, SUPERNOVA REMNANT N157B, pre-main sequence [stars], Astrophysics::Solar and Stellar Astrophysics, SPACE-TELESCOPE, Large Magellanic Cloud, 010303 astronomy & astrophysics, Physics, Nebula, Solar mass, Astrophysics::Instrumentation and Methods for Astrophysics, GRAVITATIONAL LENSING, catalogs, Magellanic, Clouds, stars: formation, stars: imaging, stars: pre-main sequence, LARGE-MAGELLANIC-CLOUD, EXPERIMENT, GALAXY EVOLUTION SAGE, ALL-SKY, SURVEY, M-CIRCLE-DOT, LUMINOSITY FUNCTION, INTERSTELLAR-MEDIUM, Astrophysics::Earth and Planetary Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometry (optics), 0103 physical sciences, Astrophysics::Galaxy Astrophysics, formation [stars], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, imaging [stars], Astrophysics - Astrophysics of Galaxies, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), star clusters: individual (30 Doradus) [galaxies], Wide Field Camera 3
Abstract

We present and describe the astro-photometric catalog of more than 800,000 sources found in the Hubble Tarantula Treasury Project (HTTP). HTTP is a Hubble Space Telescope (HST) Treasury program designed to image the entire 30 Doradus region down to the sub-solar (~0.5 solar masses) mass regime using the Wide Field Camera 3 (WFC3) and the Advanced Camera for Surveys (ACS). We observed 30 Doradus in the near ultraviolet (F275W, F336W), optical (F555W, F658N, F775W), and near infrared (F110W, F160W) wavelengths. The stellar photometry was measured using point-spread function (PSF) fitting across all the bands simultaneously. The relative astrometric accuracy of the catalog is 0.4 mas. The astro-photometric catalog, results from artificial star experiments and the mosaics for all the filters are available for download. Color-magnitude diagrams are presented showing the spatial distributions and ages of stars within 30 Dor as well as in the surrounding fields. HTTP provides the first rich and statistically significant sample of intermediate and low mass pre-main sequence candidates and allows us to trace how star formation has been developing through the region. The depth and high spatial resolution of our analysis highlight the dual role of stellar feedback in quenching and triggering star formation on the giant HII region scale. Our results are consistent with stellar sub-clustering in a partially filled gaseous nebula that is offset towards our side of the Large Magellanic Cloud., 20 pages, 22 Figures, 3 Tables, Photometric Catalogs and Mosaiced images will be available for download upon publication, accepted for publication on ApJS

Published
2015

3. Dust and Gas in the Magellanic Clouds from the HERITAGE Herschel Key Project. I. Dust Properties and Insights into the Origin of the Submm Excess Emission

Author

Mikako Matsuura, Jonathan Seale, Brian Babler, Charles W. Engelbracht, Maud Galametz, Karl D. Gordon, Kirill Tchernyshyov, Yasuo Fukui, Monica Rubio, Sacha Hony, E. Montiel, Marc Sauvage, Karl Misselt, Frédéric Galliano, Geoffrey C. Clayton, Jean-Philippe Bernard, Alberto D. Bolatto, Marta Sewilo, Remy Indebetouw, Frank P. Israel, Karin Sandstrom, Vianney Lebouteiller, Ramin A. Skibba, Annie Hughes, K. Okumura, Toshikazu Onishi, Akiko Kawamura, Pasquale Panuzzo, Katie Jameson, Martha L. Boyer, Suzanne C. Madden, Margaret Meixner, Caroline Bot, Deborah Paradis, Julia Roman-Duval, Aigen Li, Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Department of Physics and Astronomy [BatonRouge] (LSU), Louisiana State University (LSU), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of Manchester [Manchester], Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Population, FOS: Physical sciences, Astrophysics, galaxies [infrared], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], GALAXY EVOLUTION SAGE, Emissivity, Black-body radiation, Magellanic clouds, ABSORPTION-COEFFICIENT, education, ComputingMilieux_MISCELLANEOUS, CARBON ANALOG GRAINS, Physics, education.field_of_study, general [ISM], LOW-METALLICITY, ISM [infrared], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Interstellar medium, SPECTRAL ENERGY-DISTRIBUTION, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Physics and Astronomy, TEMPERATURE-DEPENDENCE, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR CLOUDS, MILKY-WAY, ULTRAVIOLET EXTINCTION, INTERSTELLAR DUST, Noise (radio), Dust emission
Abstract

The dust properties in the Large and Small Magellanic Clouds are studied using the HERITAGE Herschel Key Project photometric data in five bands from 100 to 500 micron. Three simple models of dust emission were fit to the observations: a single temperature blackbody modified by a power- law emissivity (SMBB), a single temperature blackbody modified by a broken power-law emissivity (BEMBB), and two blackbodies with different temperatures, both modified by the same power-law emissivity (TTMBB). Using these models we investigate the origin of the submm excess; defined as the submillimeter (submm) emission above that expected from SMBB models fit to observations < 200 micron. We find that the BEMBB model produces the lowest fit residuals with pixel-averaged 500 micron submm excesses of 27% and 43% for the LMC and SMC, respectively. Adopting gas masses from previous works, the gas-to-dust ratios calculated from our the fitting results shows that the TTMBB fits require significantly more dust than are available even if all the metals present in the interstellar medium (ISM) were condensed into dust. This indicates that the submm excess is more likely to be due to emissivity variations than a second population of colder dust. We derive integrated dust masses of (7.3 +/- 1.7) x 10^5 and (8.3 +/- 2.1) times 10^4 M(sun) for the LMC and SMC, respectively. We find significant correlations between the submm excess and other dust properties; further work is needed to determine the relative contributions of fitting noise and ISM physics to the correlations., 20 pages, 9 figures, accepted for publication in the ApJ

Published
2014

4. Dust and Gas in the Magellanic Clouds from the HERITAGE Herschel Key Project. II. Gas-to-dust Ratio Variations across Interstellar Medium Phases

Author

Aigen Li, Min-Young Lee, Julia Roman-Duval, Karl D. Gordon, C. Bot, Marc Sauvage, J. Seale, Aurélie Rémy-Ruyer, Frédéric Galliano, Tony Wong, Frank P. Israel, Thomas P. Robitaille, Katherine Jameson, Marta Sewilo, Maud Galametz, William T. Reach, Lister Staveley-Smith, Koryo Okumura, Monica Rubio, S. Hony, Vianney Lebouteiller, Toshikazu Onishi, Simon C. O. Glover, Alberto D. Bolatto, E. Montiel, Annie Hughes, Karl Misselt, Jean-Philippe Bernard, Brian Babler, Margaret Meixner, Geoffrey C. Clayton, Svitlana Zhukovska, Pasquale Panuzzo, Yasuo Fukui, Suzanne C. Madden, Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [BatonRouge] (LSU), Louisiana State University (LSU), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Extinction (astronomy), INFRARED OBSERVATIONS, PHYSICAL-PROPERTIES, Astrophysics, PHOTODISSOCIATION REGIONS, STAR-FORMATION, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], CO-TO-H-2 CONVERSION FACTOR, GALAXY EVOLUTION SAGE, GIANT MOLECULAR CLOUDS, ComputingMilieux_MISCELLANEOUS, molecules [ISM], Cosmic dust, Physics, COS/UVES ABSORPTION SURVEY, Star formation, extinction, Molecular cloud, SPITZER SURVEY, LOW-METALLICITY, Astronomy and Astrophysics, Galaxy, Accretion (astrophysics), Abundance of the chemical elements, Interstellar medium, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Physics and Astronomy, 13. Climate action, Space and Planetary Science, dust, structure [ISM], clouds [ISM]
Abstract

The spatial variations of the gas-to-dust ratio (GDR) provide constraints on the chemical evolution and lifecycle of dust in galaxies. We examine the relation between dust and gas at 10-50 pc resolution in the Large and Small Magellanic Clouds (LMC and SMC) based on Herschel far-infrared (FIR), H I 21 cm, CO, and Hα observations. In the diffuse atomic interstellar medium (ISM), we derive the GDR as the slope of the dust-gas relation and find GDRs of 380{sub −130}{sup +250} ± 3 in the LMC, and 1200{sub −420}{sup +1600} ± 120 in the SMC, not including helium. The atomic-to-molecular transition is located at dust surface densities of 0.05 M {sub ☉} pc{sup –2} in the LMC and 0.03 M {sub ☉} pc{sup –2} in the SMC, corresponding to A {sub V} ∼ 0.4 and 0.2, respectively. We investigate the range of CO-to-H{sub 2} conversion factor to best account for all the molecular gas in the beam of the observations, and find upper limits on X {sub CO} to be 6 × 10{sup 20} cm{sup –2} K{sup –1} km{sup –1} s in the LMC (Z = 0.5 Z {sub ☉}) at 15 pc resolution, and 4 × 10{sup 21} cm{sup –2} K{sup –1} km{sup –1} s in the SMC (Z = 0.2 Z {sub ☉})more » at 45 pc resolution. In the LMC, the slope of the dust-gas relation in the dense ISM is lower than in the diffuse ISM by a factor ∼2, even after accounting for the effects of CO-dark H{sub 2} in the translucent envelopes of molecular clouds. Coagulation of dust grains and the subsequent dust emissivity increase in molecular clouds, and/or accretion of gas-phase metals onto dust grains, and the subsequent dust abundance (dust-to-gas ratio) increase in molecular clouds could explain the observations. In the SMC, variations in the dust-gas slope caused by coagulation or accretion are degenerate with the effects of CO-dark H{sub 2}. Within the expected 5-20 times Galactic X {sub CO} range, the dust-gas slope can be either constant or decrease by a factor of several across ISM phases. Further modeling and observations are required to break the degeneracy between dust grain coagulation, accretion, and CO-dark H{sub 2}. Our analysis demonstrates that obtaining robust ISM masses remains a non-trivial endeavor even in the local Universe using state-of-the-art maps of thermal dust emission.« less

Published
2014

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