THE GREAT OBSERVATORIES ALL-SKY LIRG SURVEY: COMPARISON OF ULTRAVIOLET AND FAR-INFRARED PROPERTIES

By J. Howell, Lee Armus, J. Mazzarella, A. Evans, J. Surace, D. Sanders, A. Petric, P. Appleton, G. Bothun, C. Bridge and 14 more. 2010

140 citations recorded by the source corpus.

The Great Observatories All-sky LIRG Survey (GOALS) consists of a complete sample of 202 luminous infrared galaxies (LIRGs) selected from the IRAS Revised Bright Galaxy Sample (RBGS). The galaxies span the full range of interaction stages, from isolated galaxies to interacting pairs to late stage mergers. We present a comparison of the UV and infrared properties of 135 galaxies in GOALS observed by GALEX and Spitzer. For interacting galaxies with separations greater than the resolution of GALEX and Spitzer (∼2″–6″), we assess the UV and IR properties of each galaxy individually. The contribution of the FUV to the measured star formation rate (SFR) ranges from 0.2% to 17.9%, with a median of 2.8% and a mean of 4.0% ± 0.4%. The specific star formation rate (SSFR) of the GOALS sample is extremely high, with a median value (3.9 × 10−10 yr−1) that is comparable to the highest SSFRs seen in the Spitzer Infrared Nearby Galaxies Survey sample. We examine the position of each galaxy on the IR excess–UV slope (IRX–β) diagram as a function of galaxy properties, including IR luminosity and interaction stage. The LIRGs on average have greater IR excesses than would be expected based on their UV colors if they obeyed the same relations as starbursts with LIR < 1011 L☉ or normal late-type galaxies. The ratio of LIR to the value one would estimate from the IRX–β relation published for lower luminosity starburst galaxies ranges from 0.2 to 68, with a median value of 2.7. A minimum of 19% of the total IR luminosity in the RBGS is produced in LIRGs and ultraluminous infrared galaxies with red UV colors (β>0). Among resolved interacting systems, 32% contain one galaxy which dominates the IR emission while the companion dominates the UV emission. Only 21% of the resolved systems contain a single galaxy which dominates both wavelengths.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1ab032667742caefc47ab16354c64c183b9a6d44

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Citations in the corpus

COLD GASS, an IRAM legacy survey of molecular gas in massive galaxies - II. The non-universality of the molecular gas depletion time-scale (2011, background): “Using the measurements of stellar masses of Howell et al. (2010) and da Cunha et al. (2010) for a large sample of local LIRGs, we see that the gap in the relation that extends from the COLD GASS galaxies to the ULIRGs is filled by these galaxies of intermediate IR luminosities.”
COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, methodology): “In the specific case of the stellar masses for the GOALS LIRG/ULIRG sample used in this paper (Howell et al. 2010), this may result in an overestimate of the intrinsic stellar masses.”
SPECTRAL ENERGY DISTRIBUTIONS OF LOCAL LUMINOUS AND ULTRALUMINOUS INFRARED GALAXIES (2012, methodology): “Compared with the Howell et al. (2010) sample (with median SSFR = 3.9× 10−10 yr−1), the median SSFR of our sample is 6.8 × 10−10 yr−1, or equivalent to a mass-doubling timescale of 1.5 Gyr.”
A CHANDRA PERSPECTIVE ON GALAXY-WIDE X-RAY BINARY EMISSION AND ITS CORRELATION WITH STAR FORMATION RATE AND STELLAR MASS: NEW RESULTS FROM LUMINOUS INFRARED GALAXIES (2010, methodology): “…atlas (Jarrett et al. 2003) andKs-band extended source catalogs.8 We note that for NGC 3221, no 2MASS counterpart was available, and we therefore adopted theM⋆ estimate provided by the GOALS team (Howell et al. 2010; hereafter, H10), adjusted to match our adopted distance and IMF (see below).”
MID-INFRARED PROPERTIES OF NEARBY LUMINOUS INFRARED GALAXIES. I. SPITZER INFRARED SPECTROGRAPH SPECTRA FOR THE GOALS SAMPLE (2013, methodology): “In addition, imaging in the near-IR/optical (Hubble Space Telescope NICMOS and ACS; Haan et al. 2011, Kim et al., in prep), the UV (Galaxy Evolution Explorer nearand far-UV; Howell et al. 2010), and the X-Ray (Chandra; Iwasawa et al. 2011) are available for large subsets of the sample.”
A Herschel/PACS Far-infrared Line Emission Survey of Local Luminous Infrared Galaxies (2017, background): “…works that have already exploited the science content of multiwavelength data obtained mostly from space-born facilities including GALEX UV (Howell et al. 2010), HST optical and near-IR imaging (Haan et al. 2011; Kim et al. 2013), along with Chandra X-ray (Iwasawa et al. 2011), as well as…”
AN ATLAS OF GALAXY SPECTRAL ENERGY DISTRIBUTIONS FROM THE ULTRAVIOLET TO THE MID-INFRARED (2013, methodology): “While our sample spans a broad range of galaxy properties, some galaxy types are not included in the sample (e.g., ultra-compact dwarf galaxies) while other galaxy types (such as LIRGs) are over-represented.”
Growing supermassive black holes in the late stages of galaxy mergers are heavily obscured (2017, background): “Using the relation of Ranalli et al. (2003), we find that the star formation rate obtained for the source (∼ 54.5M⊙ yr −1, Howell et al. 2010) is able to account for the totality of the 2–10 keV luminosity observed.”
CALIBRATING EXTINCTION-FREE STAR FORMATION RATE DIAGNOSTICS WITH 33 GHz FREE–FREE EMISSION IN NGC 6946 (2011, background): “In these IR-bright starbursts, more than &90% of the UV emission can be obscured (e.g., Howell et al. 2010; Buat et al. 2010; Murphy et al. 2011).”
THE MOSDEF SURVEY: MEASUREMENTS OF BALMER DECREMENTS AND THE DUST ATTENUATION CURVE AT REDSHIFTS z ∼ 1.4–2.6 (2015, methodology): “A similar effect is seen in the comparison of UV and IR-based SFRs (e.g., Goldader et al. 2002; Reddy et al. 2010; Howell et al. 2010), where the former generally underpredict the latter for galaxies where most of the star formation occurs in optically-thick regions that are essentially “invisible”…”
Lyα EMISSION FROM GREEN PEAS: THE ROLE OF CIRCUMGALACTIC GAS DENSITY, COVERING, AND KINEMATICS (2015, background): “8 The UV slope has been shown to differ systematically depending on the adopted bandpass (Howell et al. 2010).”
C-GOALS: Chandra observations of a complete sample of luminous infrared galaxies from the IRAS Revised Bright Galaxy Survey (2011, methodology): “Similarly, IR luminosity is divided into respective components, estimated from IRAS HIRES processing (Surace et al. 2004) and new estimates based on Spitzer MIPS photometry (see Howell et al. 2010).”
EXPLAINING THE [C ii]157.7 μm DEFICIT IN LUMINOUS INFRARED GALAXIES—FIRST RESULTS FROM A HERSCHEL/PACS STUDY OF THE GOALS SAMPLE (2013, methodology): “Because > 80 − 90% of the UV and optical light of star-forming LIRGs and ULIRGs is reprocessed by dust into the IR wavelengths (Howell et al. 2010), the LIR/M⋆ ratio is equivalent to their SSFR since the SFR is directly proportional to the IR luminosity, with SFRIR/LIR =1.72× 10 −10M⊙ yr −1 L⊙ −1…”
GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies (2012, background): “Subpopulations of dusty, IR-luminous galaxies at low and high redshift are known to deviate from the original starburst relation with a higher IRX for a given slope β (Goldader et al., 2002; Chapman et al., 2005; Howell et al., 2010; Papovich et al., 2006).”
REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE (2013, unknown): “Howell et al. 2010, U et al. 2012), but to our knowledge no single study has done this consistently for all sources of interest.”