Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)

By M. Meixner, K. Gordon, R. Indebetouw, B. Whitney, M. Meade, B. Babler, J. Hora, U. Vijh, S. Srinivasan, C. Leitherer and 7 more. Proceedings of the International Astronomical Union, 2006

567 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/355034ee34a62bff36abf62f37a693a181135938

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW (2011, background): “The location of the LMC is also shown in this plot (Bernard et al. 2008).”
NEW OPTICAL REDDENING MAPS OF THE LARGE AND SMALL MAGELLANIC CLOUDS (2011, methodology): “The 160 µm maps trace emission of relatively large and cool (∼ 20 K) dust grains at larger distances from star-forming regions (Meixner et al. 2006).”
THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS). I. A CLOUD-SCALE/MULTI-WAVELENGTH VIEW OF THE INTERSTELLAR MEDIUM IN A GRAND-DESIGN SPIRAL GALAXY (2013, background): “Similarly, Bernard et al. (2008) observe an increase in dust temperature at the center of the LMC where the density of old stellar population is enhanced due to the stellar bar.”
SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). II. COOL EVOLVED STARS (2011, result): “We compare our findings to those of the SAGE survey of the Large Magellanic Cloud (SAGE-LMC; Blum et al. 2006; Meixner et al. 2006; Bonanos et al. 2009, 2010; Srinivasan et al. 2009; van Loon et al. 2010a).”
The global dust SED: tracing the nature and evolution of dust with DustEM (2010, methodology): “…the InterStellar Radiation Field (ISRF)scaling factor and the dust mass abundances (Y) for the various dust grain types, as well as constraining the size distribution of very small grains (VSGs), based on SEDs including a combination of IRAS and Spitzer data (e.g. Bernard et al. 2008; Paradis etal.”
SPITZER SAGE INFRARED PHOTOMETRY OF MASSIVE STARS IN THE LARGE MAGELLANIC CLOUD (2009, methodology): “In the mid-infrared, the Spitzer SAGE survey uniformly imaged the central 7◦ × 7◦ of the LMC in the IRAC and MIPS bands on two epochs in 2005, separated by 3 months (Meixner et al. 2006).”
DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA (2016, methodology): “Those limitations lead to large underestimates of the quantities of gas at the H I–H2 interface in our Galaxy (Grenier et al. 2005b; Ade et al. 2011; Paradis et al. 2012) as well as in the Magellanic Clouds (Bernard et al. 2008; Dobashi et al. 2008).”
The Resolved Properties of Extragalactic Giant Molecular Clouds (2008, methodology): “REFERENCES Abgrall, H., Le Bourlot, J., Pineau Des Forêts, G., Roueff, E., Flower, D. R., & Heck, L. 1992, A&A, 253, 525 Arimoto, N., Sofue, Y., & Tsujimoto, T. 1996, PASJ, 48, 275 Baumgartner, W. H., & Mushotzky, R. F. 2006, ApJ, 639, 929 Bell, T. A., Roueff, E., Viti, S., & Williams, D. A. 2006, ”
THE STAR FORMATION HISTORY OF THE LARGE MAGELLANIC CLOUD (2009, background): “Most dramatically, the bar is absent in images that trace the interstellar medium of the LMC, such as HI (Kim et al. 1998), Hα (Points 2008), CO (Mizuno et al. 2001), or 8µm and 24µm emission (Meixner et al. 2006).”
CARNEGIE HUBBLE PROGRAM: A MID-INFRARED CALIBRATION OF THE HUBBLE CONSTANT (2012, methodology): “LMC data for stars with P < 6 days from Meixner et al. (2006) are also plotted, but not included in the fits.”
THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP (2011, methodology): “It cannot recover a pervasive, CO-free H2 component like that suggested for the LMC by Bernard et al. (2008).”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, background): “First, as discussed by Bernard et al. (2008), there are residual foreground Galactic filamentary structures.”
THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD POPULATION OF THE LARGE MAGELLANIC CLOUD (2011, background): “…to H2 mass is likely to decrease on larger spatial scales (Israel 2000), and studies of LMC dust emission at far-infrared wavelengths (e.g., Bernard et al. 2008; Roman-Duval et al. 2010) suggest the presence of more dust than can be accounted for using standard conversion factors for HI…”
THE SPITZER–WISE SURVEY OF THE ECLIPTIC POLES (2011, methodology): “Suffering from small sample fluctuation, the bright end, S(24 μm) > 6 mJy, shows an excess (relative to SWIRE) that is likely due to foreground Milky Way and LMC stars that have not been removed with the color thresholding.”