Multiwavelength Observations of Dusty Star Formation at Low and High Redshift

By K. Adelberger, C. Steidel. 2000

328 citations recorded by the source corpus.

If high-redshift galaxies resemble rapidly star-forming galaxies in the local universe, most of the luminosity produced by their massive stars will have been absorbed by dust and reradiated as far-infrared photons that cannot be detected with existing facilities. This paper examines what can be learned about high-redshift star formation from the small fraction of high-redshift galaxies' luminosities that is emitted at accessible wavelengths. We first consider the most basic ingredient in the analysis of high-redshift surveys: the estimation of star formation rates for detected galaxies. Standard techniques require an estimate of the bolometric luminosity produced by their massive stars. We review and quantify empirical correlations between bolometric luminosities produced by star formation and the UV, mid-IR, sub-mm, and radio luminosities of galaxies in the local universe. These correlations suggest that observations of high-redshift galaxies at any of these wavelengths should constrain their star formation rates to within ~0.2-0.3 dex. We assemble the limited evidence that high-redshift galaxies obey these locally calibrated correlations. The second part of the paper assesses whether existing surveys have found the galaxies that host the majority of star formation at high redshift even though they directly detect only a small fraction of the luminosities of individual galaxies. We describe the characteristic luminosities and dust obscurations of galaxies at z ~ 0, z ~ 1, and z ~ 3. After discussing the relationship between the high-redshift populations selected in surveys at different wavelengths, we calculate the contribution to the 850 μm background from each and argue that these known galaxy populations can together have produced the entire observed background. The available data show that a correlation between star formation rate and dust obscuration Lbol,dust/LUV exists at low and high redshift alike. The existence of this correlation plays a central role in the major conclusion of this paper: most star formation at high redshift occurred in galaxies with moderate dust obscurations 1 ≲ Lbol,dust/LUV ≲ 100 similar to those that host the majority of star formation in the local universe and to those that are detected in UV-selected surveys.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fa5b1d36308af0d3e35421f0b7f9cde44081d0a9

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Citations in the corpus

Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate (2005, methodology): “…of IR/UV and the trend with total luminosity in the z 0:7 sample is very similar to that observed in the local universe (e.g., Wang & Heckman 1996; Adelberger & Steidel 2000; Bell 2003), indicating little or no evolution in the relative proportion of obscured star formation at least to z 0:7.17…”
Galaxy Size Evolution at High Redshift and Surface Brightness Selection Effects: Constraints from the Hubble Ultra Deep Field (2004, background): “0.45 applied to a 108 yr burst) and some evolved galaxies (Franx et al. 2003) though the former objects are expected to be rare (Adelberger & Steidel 2000).”
The Direct Detection of Lyman Continuum Emission from Star-forming Galaxies at z~3 (2006, methodology): “For this estimate, we use 〈f1500/f900,corr 〉 to convert the published LBG 1500 Å luminosity function (Adelberger & Steidel 2000) to one at 900 Å.”
Did most present-day spirals form during the last 8 Gyr? - A formation history with violent episodes revealed by panchromatic observations (2004, methodology): “By comparing these corrections to IR fluxes of z ∼ 0.9 ISO galaxies from Flores et al. (1999), Adelberger & Steidel (2000) claimed that their method appears to work within a factor 3 (see also Adelberger 2001).”
Spitzer View on the Evolution of Star-forming Galaxies from z = 0 to z ~ 3 (2005, result): “Attenuations of the same order (factors of 5–10) have also been found by other authors (Madau et al. 1998; Steidel et al. 1999; Adelberger & Steidel 2000; Massarotti et al. 2001; Schiminovich et al. 2005, among others).”
Ultradeep Near-Infrared ISAAC Observations of the Hubble Deep Field South: Observations, Reduction, Multicolor Catalog, and Photometric Redshifts (2002, background): “…confirmed at ze2 and have been subject to targeted studies on spatial clustering (Giavalisco & Dickinson 2001), internal kinematics (Pettini et al. 1998, 2001), dust properties (Adelberger & Steidel 2000), and stellar composition (Shapley et al. 2001; Papovich, Dickinson, & Ferguson 2001).”
UV LUMINOSITY FUNCTIONS AT REDSHIFTS z ∼ 4 TO z ∼ 10: 10,000 GALAXIES FROM HST LEGACY FIELDS (2014, background): “In the rest-frame UV , the luminosity of galaxies strongly correlates with the star formation rates for all but the most dust-obscured galaxies (e.g., Wang & Heckman 1996; Adelberger & Steidel 2000; Martin et al. 2005b).”
Star formation and mass assembly in high-redshift galaxies (2009, background): “As expected, the only galaxies fitted by early-type SEDs (red crosses) have very faint 24µm emission.”
UV-CONTINUUM SLOPES AT z ∼ 4–7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR–MAGNITUDE RELATIONSHIP FOR z ⩾ 4 STAR-FORMING GALAXIES (2011, methodology): “The earliest analyses were at z ∼ 2- 3 using either ground-based observations (Steidel et al. 1999; Adelberger & Steidel 2000) or the deep WFPC2 observations over the HDF North (Meurer et al. 1999).”
Rest-Frame Ultraviolet Spectra of z ∼ 3 Lyman Break Galaxies (2003, methodology): “Based on the range of UV colors of LBGs, and the types of assumptions described above, Adelberger & Steidel (2000) find that the UV luminosities of LBGs are attenuated on average by a factor of∼ 7 due to dust extinction, and that this factor ranges from 0− 100.”
Star Formation and Extinction in Redshift z~2 Galaxies: Inferences from Spitzer MIPS Observations (2006, methodology): “A third possibility, and one that is suggested by the results of this paper and other studies (e.g., Adelberger & Steidel 2000; Calzetti & Heckman 1999), is that the dust obscuration of galaxies at a given bolometric luminosity changes as a function of redshift, a result that may reflect dust…”
A STEEP FAINT-END SLOPE OF THE UV LUMINOSITY FUNCTION AT z ∼ 2–3: IMPLICATIONS FOR THE GLOBAL STELLAR MASS DENSITY AND STAR FORMATION IN LOW-MASS HALOS (2008, methodology): “…suppressing star formation in high mass halos (Croton et al. 2006; Scannapieco et al. 2005; Granato et al. 2004), even after taking into account the saturation of UV light with respect to the total star formation rates of galaxies with large SFRs (Adelberger & Steidel 2000; Reddy et al. 2006b).”
A New Photometric Technique for the Joint Selection of Star-forming and Passive Galaxies at 1.4 ≲ z ≲ 2.5 (2004, background): “The UV-selection requires the UV continuum to be relatively flat, thus limiting the overall dust extinction toE(B − V ) <∼ 0.3 (Adelberger & Steidel 2000), while many of the K20 galaxies atz > 1.4 are more reddened (see Fig.”
The evolution of the luminosity functions in the FORS Deep Field from low to high redshift: I. The blue bands (2004, background): “…to derive luminosity functions at different redshifts in the ultraviolet (UV) (Treyer et al., 1998; Steidel et al., 1999; Cowie et al., 1999; Adelberger & Steidel, 2000; Cohen et al., 2000; Sullivan et al., 2000; Ouchi et al., 2001; Poli et al., 2001; Wilson et al., 2002; Wolf et al., 2003;…”
Dusty Star Forming Galaxies at High Redshift (2014, methodology): “…et al. find that, much worse than the 10× extinction in the rest-optical, the UV luminosities of SMGs underestimate the far-infrared star formation rates by a median factor of ∼120, even after nominal dust-correction via the prescriptions of Meurer et al. (1997) and Adelberger and Steidel (2000).”
Escape of Ionizing Radiation from High-Redshift Galaxies (2007, methodology): “Both Giallongo et al. (2002) and Shapley et al. (2006) measurements are corrected from the relative measurements of the ratiofesc(912)/ fesc(1500) they report to the absolute measurement offesc(912) by adopting a value of fesc(1500) = 0.2 from Adelberger & Steidel (2000).”
Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV Luminosity Functions at $z \sim 4-7$ Derived with the Half-Million Dropouts on the 100 deg$^2$ Sky (2017, background): “…2006), inefficiency of gas cooling in high- mass dark matter haloes (e.g., Binney 1977; Rees & Ostriker 1977; Silk 1977; Benson et al. 2003), and dust attenuation, which becomes substantial for the most luminous galaxies (e.g., Wang & Heckman 1996; Adelberger & Steidel 2000; Martin et al. 2005).”
z ~ 7-10 Galaxies in the HUDF and GOODS Fields: UV Luminosity Functions (2008, background): “As a result, the UV luminosity of star-forming galaxies does not tend to reach above some maximum value (see discussion in e.g., Adelberger & Steidel 2000; Martin el al.”