THE FMOS-COSMOS SURVEY OF STAR-FORMING GALAXIES AT z ∼ 1.6. I. Hα-BASED STAR FORMATION RATES AND DUST EXTINCTION

By D. Kashino, J. Silverman, G. Rodighiero, A. Renzini, N. Arimoto, E. Daddi, S. Lilly, D. Sanders, J. Kartaltepe, H. Zahid and 19 more. 2013

154 citations recorded by the source corpus.

We present the first results from a near-IR spectroscopic survey of the COSMOS field, using the Fiber Multi-Object Spectrograph on the Subaru telescope, designed to characterize the star-forming galaxy population at 1.4 < z < 1.7. The high-resolution mode is implemented to detect Hα in emission between 1.6–1.8 μm with fHα ≳ 4 × 10−17 erg cm−2 s−1. Here, we specifically focus on 271 sBzK-selected galaxies that yield a Hα detection thus providing a redshift and emission line luminosity to establish the relation between star formation rate and stellar mass. With further J-band spectroscopy for 89 of these, the level of dust extinction is assessed by measuring the Balmer decrement using co-added spectra. We find that the extinction (0.6 ≲ AHα ≲ 2.5) rises with stellar mass and is elevated at high masses compared to low-redshift galaxies. Using this subset of the spectroscopic sample, we further find that the differential extinction between stellar and nebular emission Estar(B − V)/Eneb(B − V) is 0.7–0.8, dissimilar to that typically seen at low redshift. After correcting for extinction, we derive an Hα-based main sequence with a slope (0.81 ± 0.04) and normalization similar to previous studies at these redshifts.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/95992404229293268c856d99c63ef5964d99cb6d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. P. V. van Dokkum
4. D. M. Alexander
5. R. Dav'e
6. A. Dekel
7. M. Franx
8. E. Daddi

In Instrumentation

1. P. V. van Dokkum
2. M. Franx
3. P. Hopkins
4. L. Hernquist
5. A. Dekel
6. C. Conroy
7. E. Daddi
8. A. Renzini

Citations in the corpus

• The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, methodology): “We assume for nebular emission the same dust attenuation as for stars (Reddy et al. 2010; Kashino et al. 2013) although the issue is still debated (Förster Schreiber et al. 2009; Wuyts et al. 2013).”
• The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, background): “…be exacerbated if the Hα emission from the H II regions were more attenuated relative to the stellar continuum light along the line-of-sight (e.g., Calzetti et al. 2000; FS09; M11; Ly et al. 2012; Wuyts et al. 2013; Kashino et al. 2013; Price et al. 2014; Koyama et al. 2015; Puglisi et al. 2016).”
• AN OBJECTIVE DEFINITION FOR THE MAIN SEQUENCE OF STAR-FORMING GALAXIES (2015, methodology): “Many subsequent studies have followed, confirming the existence of a MS, all the way to at least z ∼ 4 (Bernhard et al. 2014; Karim et al. 2011; Kashino et al. 2013; Magnelli et al. 2014; Pannella et al. 2009; Peng et al. 2010, hereafter P10; Popesso et al. 2011, 2012; Rodighiero et al. 2010, 2011,…”
• CO excitation of normal star forming galaxies out to $z=1.5$ as regulated by the properties of their interstellar medium (2014, background): “However, the difference between the attenuation of the HII regions and the stellar continuum appe rs to be reduced with respect to the local Universe (Kashino et al 2013; Price et al 2013; Pannella et al 2014).”
• X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects (2014, methodology): “…by two other samples we will use in the following as comparison: the green area marks the locus occupied by the 8 massive star forming galaxies presented in Förster Schreiber et al. (2014), while the black area mark the mass range of MS star forming galaxies presented in Kashino et al. (2013).”
• A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, unknown): “…(K11); Shim et al. 2011 (S11); Bouwens et al. 2012 (B12); Whitaker et al. 2012 (W12); Zahid et al. 2012 (Z12); Lee et al. 2012 (L12); Reddy et al. 2012b (R12); Salmi et al. 2012 (S12); Moustakas et al. 2013 (M13); Kashino et al. 2013 (K13); Sobral et al. 2014 (So14); Steinhardt et al. 2014, subm.”
• A TURNOVER IN THE GALAXY MAIN SEQUENCE OF STAR FORMATION AT M* ∼ 1010 M☉ FOR REDSHIFTS z < 1.3 (2015, methodology): “…using emission lines combined with reddening corrections to infer the dustcorrected SFR (Brusa et al. 2010; Sobral et al. 2012; Zahid et al. 2012; Kashino et al. 2013) or measuring the UV or optical emission from young massive stars and correcting for the radiation lost to dust obscuration (Lee…”
• THE MOSDEF SURVEY: MEASUREMENTS OF BALMER DECREMENTS AND THE DUST ATTENUATION CURVE AT REDSHIFTS z ∼ 1.4–2.6 (2015, background): “The advances enabled with the new generation of multi-object near-IR spectrographs on 8-10 m-class telescopes have begun to remedy these past deficiencies in high-redshift near-IR spectroscopy (e.g., Kashino et al. 2013; Steidel et al. 2014).”
• GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, methodology): “…respectively, while we use the same Calzetti et al. (2000) extinction curve for both emissions. the redshift evolution, at least up toz ≃1.5, of theAHα–logM∗ relation (e.g., Sobral et al. 2012; Domínguez et al. 2013; Ibar et al. 2013; Kashino et al. 2013; Momcheva et al. 2013; Price et al. 2014).”
• An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source (2015, unknown): “…ratio between Balmer lines is compared with the expected ratio derived from theory (e.g., Hα/Hβ = 2.86; Osterbrock 1989), and assuming an attenuation curve, the dust correction is derived at any wavelength (e.g., Kashino et al. 2013; Domı́nguez et al. 2013; Price et al. 2014; Steidel et al. 2014).”
• Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, methodology): “The same attenuation value is used for the stellar and nebular components (e.g., Erb et al. 2006; Kashino et al. 2013).”
• RECONCILING THE STELLAR AND NEBULAR SPECTRA OF HIGH-REDSHIFT GALAXIES (2016, background): “There is a rapidly developing literature comparing dust attenuation factors estimated from nebular line ratios to those estimated from continuum reddening (e.g., Calzetti et al. 2000; Kashino et al. 2013; Price et al. 2014; Reddy et al. 2015; Shivaei et al. 2016).”
• CONSTRAINING THE LOW-MASS SLOPE OF THE STAR FORMATION SEQUENCE AT 0.5 < z < 2.5 (2014, background): “We do not find evidence for a strong evolution in the average dust properties of galaxies at 0.5 < z < 2.5, although galaxies at z > 1 do appear to have different dust properties than local starburst galaxies (see also, e.g., Kashino et al. 2013; Price et al. 2014).”