The Luminosity Function and Star Formation Rate between Redshifts of 0.07 and 1.47 for Narrowband Emitters in the Subaru Deep Field

By C. Ly, M. Malkan, N. Kashikawa, K. Shimasaku, M. Doi, Tohru Nagao, M. Iye, T. Kodama, T. Morokuma, K. Motohara. 2006

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SDF line-emitting galaxies in four narrowband filters at low and intermediate redshifts are presented. Broadband colors, follow-up optical spectroscopy, and multiple NB filters are used to distinguish Hα, [O II], and [O III] emitters at z = 0.07-1.47 to construct their LFs. These LFs are derived down to faint magnitudes, allowing for an accurate determination of the faint-end slope. With a large (N ~ 200-900) sample for each redshift interval, a Schechter profile is fitted to each LF. Prior to dust extinction corrections, the [O III] and [O II] LFs agree reasonably well with those of Hippelein et al. The z = 0.08 Hα LF, which reaches 2 orders of magnitude fainter than Gallego et al., is steeper by 25%. This indicates that there are more low-luminosity star-forming galaxies for z < 0.1. The faint-end slope α and ϕ⋆ show a strong redshift evolution, while L⋆ shows little evolution. The evolution in α indicates that low-luminosity galaxies have a stronger evolution compared to brighter ones. Integrated SFR densities are derived via Hα, [O III], and [O II] for 0.07 < z < 1.47. A steep increase in the SFR density, as a function of redshift, is seen for 0.4 < z < 0.9. For z > 1, the SFR densities are similar. The latter is consistent with previous UV and [O II] measurements. Below z < 0.4, the SFR densities are consistent with several Hα, [O II], and UV measurements, but others are a factor of 2 higher. For example, the z = 0.066-0.092 LF agrees with Jones & Bland-Hawthorn, but at z = 0.24 and 0.40, their number densities are twice as high. This discrepancy can be explained by cosmic variance.

Subfields: Astronomy and Astrophysics, Instrumentation

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HiZELS: a high-redshift survey of Hα emitters – I. The cosmic star formation rate and clustering at z= 2.23 (2008, background): “2003; Pascual et al. 2005; Ly et al. 2007) for SFR estimates.”
A large Hα survey at z = 2.23, 1.47, 0.84 and 0.40: the 11 Gyr evolution of star-forming galaxies from HiZELS (2012, methodology): “The best-fit functions and their errors are also shown in Figure 7, together with the z ≈ 0 luminosity function determined by Ly et al. (2007) – which has extended the work by Gallego et al. (1995) at z ≈ 0, for a local-Universe comparison.”
Kinematics and history of the solar neighbourhood revisited (2009, background): “The cosmic SF rate peaked at redshifts 1–2 (e.g. Ly et al. 2007), which in the concordance cosmology corresponds to look-back times between 7.8 and 10.5 Gyr.”
DUST EXTINCTION FROM BALMER DECREMENTS OF STAR-FORMING GALAXIES AT 0.75 ⩽ z ⩽ 1.5 WITH HUBBLE SPACE TELESCOPE/WIDE-FIELD-CAMERA 3 SPECTROSCOPY FROM THE WFC3 INFRARED SPECTROSCOPIC PARALLEL SURVEY (2012, result): “Our results are compatible with the claims by Sobral et al. (2012) that an L∗ galaxy13 at z ∼ 1 (between 1042.25 and 1042.50 erg s−1, Sobral et al. 2012) has the same dust extinction as an L∗ galaxy today (approximately 10 41.20 erg s−1, Ly et al. 2007).”
VERY STRONG EMISSION-LINE GALAXIES IN THE WFC3 INFRARED SPECTROSCOPIC PARALLEL SURVEY AND IMPLICATIONS FOR HIGH-REDSHIFT GALAXIES, (2011, background): “Many of the faint WISP galaxies have strong [Oiii] λ5007 emission, and often weak [Oii] λ3727 emission, with a median ratio of ([Oiii] λ5007/[Oii] λ3727) = 2.5 (see also Hicks et al. 2002; Maier et al. 2006; Ly et al. 2007), suggestive of low metal abundances (Log(O/H) .”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, background): “As a result, [O ii]-based SFR estimates are available for tens of thousands of galaxies at z ∼ 0.1–1.5 (e.g., Franzetti et al. 2007; Ly et al. 2007; Cooper et al. 2008).”
Star formation at z=1.47 from HiZELS: an Hα+[O ii] double-blind study* (2011, methodology): “13, together with the luminosity functions determined by Ly et al. (2007) – extending the work by Gallego et al. (1995) – at z ≈ 0 and that from Shioya et al. (2008) at z = 0.24.”
HiZELS:a high-redshift survey of Hα emitters - II. the nature of star-forming galaxies at z = 0.84 (2009, methodology): “However, evidence for a steep faint-end slope in the Hα luminosity function (α ∼ −1.6) has been found even at z = 0.08 by Ly et al. (2007) as well as in other Hα studies at higher redshifts, z ∼ 0.2–1.3 (e.g. Hopkins et al. 2000; Fujita et al. 2003; Dale et al. 2008).”
Evolution in the properties of Lyman-α emitters from redshifts z ~ 3 to z ~ 2 (2008, methodology): “To this limit, Ly et al. (2007) detected∼ 0.2 emitters per Mpc−3, corresponding to approximately 160 objects in our survey volume, of which only 2% are expected to have an EW larger than the selection criteria limit of EWobs = 65 Å (Hogg et al. 1998).”
The dependence of star formation activity on environment and stellar mass at z∼ 1 from the HiZELS-Hα survey (2010, background): “This has led to significant progress (e.g. Ly et al. 2007; Shioya et al. 2008; Geach et al. 2008; Sobral et al. 2009a; Garn et al. 2010; Sobral et al. 2010) taking advantage of large samples of typically hundreds of Hα emitters up to z = 2.23.”