The Magellanic Clouds Photomtric Survey: The Small Magellanic Cloud Stellar Catalog and Extinction Map

By Dennis Zaritsky, J. Harris, I. Thompson, E. Grebel, Philip Massey. 2001

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We present our catalog of U, B, V, and I stellar photometry of the central 18 deg2 area of the Small Magellanic Cloud. We combine our data with the Two Micron All Sky Survey and Deep Near-Infrared Southern Sky Survey (DENIS) catalogs to provide, when available, U through Ks data for stars. Internal and external astrometric and photometric tests using existing optical photometry (U, B, and V from Massey's bright star catalog; B, V, and I from the microlensing database of OGLE; and I from the near-infrared sky survey DENIS) are used to determine the observational uncertainties and identify systematic errors. We fit stellar atmosphere models to the optical data to check the consistency of the photometry for individual stars across the passbands and to estimate the line-of-sight extinction. Finally, we use the estimated line-of-sight extinctions to produce an extinction map across the Small Magellanic Cloud, and we investigate the nature of extinction as a function of stellar population.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a80f2e275b38cf98a807dd2e25429e8effa0d70f

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MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “The very wide baseline in wavelength— optical UBV I from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 2002) all the way out to 160 µm from Spitzer/MIPS—allows for accurate photometric classification of AGB subtypes and identification of contaminants such as unresolved background…”
Ten eclipsing binaries in the Small Magellanic Cloud: fundamental parameters and SMC distance (2002, background): “(e.g., Hill, Madore & Freedman 1994; Massey et al. 1995; Dutra et al. 2001; Zaritsky et al. 2002).”
Mass loss of stars on the asymptotic giant branch (2018, background): “…and the completeness of the estimated mass-loss rates for objects in the Magellanic Clouds (MCs) have improved significantly due to the large surveys performed, e.g., MCPS (Zaritsky et al. 2004), 2MASS (Skrutskie et al. 2006), SAGE (Meixner et al. 2006), and AKARI IRC Survey (Ita et al. 2008).”
Optical Star Formation Rate Indicators (2005, neutral): “…stellar continuum experiences a fraction of the dust attenuation suffered by star-forming regions (MK06; Calzetti et al. 1994; Kennicutt et al. 1994; Mayya & Prabhu 1996; Calzetti 1997; Charlot & Fall 2000; Poggianti &Wu 2000; Poggianti et al. 2001; Stasińska & Sodré 2001; Zaritsky et al. 2002).”
Empirical color transformations between SDSS photometry and Other photometric systems. (2005, neutral): “(1999); Zaritsky et al. (2002, 2004); Skrutskie et al. (2006).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, background): “We expect the ratio of dust luminosity to ionizing luminosity to be less sensitive to these age differences, however, because the attenuation of a given population decreases with increasing stellar age (e.g., Zaritsky et al. 2002).”
Massive Stars in the Local Group: Implications for Stellar Evolution and Star Formation (2003, background): “…very deep, and is providing important new data on the star-formation histories of the Clouds, but unfortunately saturates at magnitudes where massive stars dominate, as well as having calibration problems atU, which have only been partially addressed (compare Zaritsky et al. 2002, Massey 2002a).”
AGE DETERMINATION OF SIX INTERMEDIATE-AGE SMALL MAGELLANIC CLOUD STAR CLUSTERS WITH HST/ACS (2008, neutral): “A spatial projection of the clusters’ location towards the SMC (red circles) is shown in Figure 1 superimposed on a star map of the SMC generated using the point source catalog of the Small Magellanic Cloud Photometric Survey (Zaritsky et al. 2002) for stars V<16.5 mag.”
The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, background): “Massey (2002) and Zaritsky et al. (2004) obtained higher magnitudes of V = 12.84 mag and V = 12.9 mag, respectively.”
Bump Cepheids in the Magellanic Clouds: Metallicities, the Distances to the LMC and SMC, and the Pulsation-Evolution Mass Discrepancy (2006, background): “The studies of Zaritsky (1999) and Zaritsky et al. (2002) describes this systematic effect in more detail.”
Spitzer SAGE Survey of the Large Magellanic Cloud. II. Evolved Stars and Infrared Color-Magnitude Diagrams (2006, background): “SAGE builds on and leverages a wealth of past observations of evolved stars in the LMC. Optical (Magellanic Cloud Photometric Survey; see Zaritsky et al. 2004)23 and near-infrared surveys—for example, DENIS (Epchtein et al. 1994) and the Two Micron All Sky Survey (2MASS; Skrutskie et al. 2006)—…”
A New Look at the Kinematics of Neutral Hydrogen in the Small Magellanic Cloud (2003, methodology): “Zaritsky et al. (2002) found E(B V ) 0.05–0.25 mag.”
THE STAR FORMATION HISTORY OF THE LARGE MAGELLANIC CLOUD (2009, methodology): “We have already applied StarFISH to the MCPS catalog of the Small Magellanic Cloud (SMC, Harris & Zaritsky 2004), and the present analysis will be similar to that work; all important differences are noted in this Section.”
The Origin of the Magellanic Stream and Its Leading Arm (2007, background): “…2006; S3MC: Bolatto et al. 2007), in the nearinfrared (DENIS: Epchtein et al. 1997; 2MASS: Skrutskie et al. 2006), in broadband optical colors (MCPS: Zaritsky et al. 2002, 2004) as well as in optical emission lines (MCELS: Smith et al. 1998), and at ultraviolet (Smith, Cornett & Hill 1987) and…”
SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). II. COOL EVOLVED STARS (2011, methodology): “The SAGE-SMC catalog includes optical UBV I photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 2002), JHKs photometry from the 2-Micron All Sky Survey (2MASS; Skrutskie et al. 2006) and the InfraRed Survey Facility survey (IRSF; Kato et al. 2007), mid-IR photometry…”
A UBVR CCD Survey of the Magellanic Clouds (2001, methodology): “The recent paper by Zaritsky et al. (2002) made use of our uncorrected U B photometry to fix their own transformation problems; this should work well for the fainter dwarfs in their survey.”
Star Formation in NGC 5194 (M51a): The Panchromatic View from GALEX to Spitzer (2005, background): “This problem is exacerbated by the fact that populations of different ages suffer different amounts of dust extinction (Calzetti, Kinney & Storchi– Bergmann 1994; Charlot & Fall 2000; Zaritsky et al. 2004).”