Far-Infrared Galaxies in the Far-Ultraviolet

By J. Goldader, G. Meurer, T. Heckman, M. Seibert, D. Sanders, D. Calzetti, Charles C. Steidel U. Pennsylvania, Jhu, IfA Hawaii, Stsci and 1 more. 2001

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In an effort to better understand the UV properties of ultraluminous infrared galaxies (ULIGs), and compare them to the rest-frame UV properties of high redshift submillimeter and Lyman-break galaxies, we have obtained far- and near-UV imaging observations (λeff = 1457 and 2364 Å, respectively) of two luminous infrared galaxies (LIGs-VV 114 and IC 883) and five ULIGs (IRAS 08572+3915, Mrk 273, IRAS 15250+3609, Arp 220, and IRAS 19254-7245) using the Hubble Space Telescope. All the galaxies were detected in both channels. UV light, both diffuse and from star clusters, can be traced to within the inner kiloparsec of the dominant near-IR nuclei. However, in general, the brightest UV sources are clearly displaced from the I-band and near-IR peaks by at least hundreds of parsecs. Furthermore, only 0.07%-7.3% of the total near-UV light is projected within the inner 500 pc radius, even though this is the same region where most of the bolometric energy is generated. All nuclei are highly obscured by dust. Even after correction for dust reddening, the global UV emission fails to account for the total bolometric luminosities of these systems by factors of 3-75. The discrepancy is much worse if only the central regions, where the bolometric luminosities are generated, are included. In two cases (VV 114 and IRAS 08572+3915), the merging companion galaxies are more prominent in the UV than the more IR luminous member. While all our galaxies show possible signatures of active galactic nucleus (AGN) activity, only IRAS 19254-7245 yields even a possible detection of an AGN in our UV images. Simple calculations show that all but one of our galaxies would be expected to drop below the detection thresholds of, e.g., the Hubble Deep Fields at redshifts between 1.5 and 3, and we find that ~2 of our five ULIGs would be selected as extremely red objects in this redshift range. A typical ULIG in our sample would be too faint to be detected at high redshift in the deepest current optical or submillimeter deep surveys. Only VV 114 has UV luminosity and color similar to Lyman-break galaxies at z ~ 3; the other galaxies would be too faint and/or red to be selected by current surveys. The low UV brightnesses of our ULIGs mean that they would not appear as optically bright (or bright ERO) submillimeter galaxy counterparts, although they might be similar to the fainter submillimeter galaxy counterparts.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

• DUST OBSCURATION AND METALLICITY AT HIGH REDSHIFT: NEW INFERENCES FROM UV, Hα, AND 8 μm OBSERVATIONS OF z ∼ 2 STAR-FORMING GALAXIES (2010, unknown): “11 Goldader et al. 2002).”
• THE MULTIPHASE STRUCTURE AND POWER SOURCES OF GALACTIC WINDS IN MAJOR MERGERS (2013, background): “Most of the UV light in ULIRGs is heavily obscured by concentrations of nuclear dust (Soifer et al. 2000; Goldader et al. 2002); however, on larger scales outflowing dust may play an important role as a foreground screen in extinguishing the visible continuum.”
• ON STAR FORMATION RATES AND STAR FORMATION HISTORIES OF GALAXIES OUT TO z ∼ 3 (2011, background): “Finally, we note that ultra-deep IRS spectroscopy of z ∼ 1 LIRGs and z ∼ 2 ULIRGs (Fadda et al. 2010) found that both categories are starburst dominated.”
• THE GREAT OBSERVATORIES ALL-SKY LIRG SURVEY: COMPARISON OF ULTRAVIOLET AND FAR-INFRARED PROPERTIES (2010, methodology): “…have different effective wavelengths than previous instruments such as IUE or STIS, the normalization of β(GALEX) is different from previous work (e.g., Meurer et al. 1999; Goldader et al. 2002; see Appendix A for a more detailed discussion and a direct conversion between β(GALEX) and β(IUE)).”
• The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, background): “…et al. 2011; Rodighiero et al. 2014), it has been shown for example that these corrections cannot recover the full SFR of the most active objects (Goldader et al. 2002; Buat et al. 2005; Elbaz et al. 2007; Rodighiero et al. 2011, 2014; Wuyts et al. 2011; Penner et al. 2012; Oteo et al. 2013).”
• The GALEX Ultraviolet Atlas of Nearby Galaxies (2006, background): “…is valid only when applied to UV-selected starburst galaxies but not in the case of infrared-bright objects like the luminous/ultraluminous infrared galaxies (LIRGs/ULIRGs; Goldader et al. 2002) or even for normal spiral or irregular galaxies (see Bell et al. 2002 for results on the LMC).”
• THE CALIBRATION OF MONOCHROMATIC FAR-INFRARED STAR FORMATION RATE INDICATORS (2010, background): “…galaxies, but will lose accuracy both at the low end and high end of the SFSD range (Calzetti, Kinney & Storchi–Bergmann 1994; Meurer, Heckman & Calzetti 1999; Calzetti et al. 2000; Buat et al. 2002; Goldader et al. 2002; Bell 2003; Buat et al. 2005; Calzetti et al. 2005; Seibert et al. 2005).”
• 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).”
• 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”…”
• Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth (2007, background): “Even more importantly, it is well known that strongest starbursts are opaque to UV radiation and its total SFR activity cannot be reliably estimated solely from the UV, even after reddening corrections (e.g., Goldader et al. 2002; Buat et al. 2005).”
• THE CHARACTERISTIC STAR FORMATION HISTORIES OF GALAXIES AT REDSHIFTS z ∼ 2–7 (2012, background): “…Calzetti et al. (2000) dust corrections for such objects are typically too low due to the fact that much of the star formation is completely obscured by dust, and hence the UV slope decouples from extinction for such highly obscured galaxies (e.g., Goldader et al. 2002; Reddy et al. 2006b, 2010).”
• Star Formation and Extinction in Redshift z~2 Galaxies: Inferences from Spitzer MIPS Observations (2006, background): “The local sample includes the ULIRGs studied byGoldader et al. (2002).”
• A study of the gas–star formation relation over cosmic time (2010, background): “The far-UV luminosity is even more sensitive to extinction than Hα, and for this reason it fails in the case of very dusty SFGs (Goldader et al. 2002).”
• The Physical Nature of Rest-UV Galaxy Morphology during the Peak Epoch of Galaxy Formation (2006, unknown): “In the case of VV 114, near-IR imaging (Goldader et al. 2002) indicates that all of the clumps of UV emission are associated with only one galaxy of the merger pair and that the multi-component UV morphology therefore directly reflects clumpy star formation rather than tracing tidally distorted…”
• The Rest-Frame Far-Ultraviolet Morphologies of Star-Forming Galaxies at z ~ 1.5 and 4 (2006, background): “Bright starforming regions of local galaxies may appear as several distinct objects when viewed in the FUV (e.g., Goldader et al. 2002).”
• DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS (2011, background): “For (U)LIRGs, Howell et al. (2010; see also Goldader et al. 2002; Calzetti 2001) showed that (U)LIRGs in the Great Observatories ALL-sky LIRG Survey (GOALS) lie above the starburst relation, and the correlation between IRX and FUV-NUV color is not strong either.”
• Spitzer Observations of Massive, Red Galaxies at High Redshift (2005, background): “In local ULIRGs the geometry of the forming star clusters and dust is highly complex.”