FMOS near-IR spectroscopy of<i>Herschel</i>-selected galaxies: star formation rates, metallicity and dust attenuation at<i>z</i>∼ 1

Roseboom, I. G.; Bunker, A. J.; Sumiyoshi, Masanao; Wang, L.; Dalton, Gavin; Akiyama, Masayuki; Bock, J. J.; Bonfield, D. G.; Buat, V.; Casey, Caitlin M.; Chapin, Edward L.; Clements, D. L.; Conley, A.; Curtis-Lake, Emma; Cooray, Asantha; Dunlop, James; Farrah, D.; Ham, S. J.; Ibar, E.; Iwamuro, Fumihide; Kimura, Masahiko; Lewis, Ian; Macaulay, E.; Magdis, G.; Maihara, Toshinori; Marsden, G.; Mauch, T.; Moritani, Yuuki; Ohta, Kouji; Oliver, Seb; Page, M. J.; Schulz, B.; Scott, D.; Symeonidis, M.; Takato, Naruhisa; Tamura, Naoyuki; Totani, Tomonori; Yabe, Kiyoto; Zemcov, Michael

doi:10.1111/j.1365-2966.2012.21777.x

Cited by 38 publications

(36 citation statements)

References 80 publications

(129 reference statements)

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“…These results are consistent with those of Kocevski et al (2011a), in which it was observed that, for Spitzer/MIPS selected galaxies in a large-scale structure at z ∼ 0.9, the nebular extinction increased with increasing L TIR . These results are also broadly consistent with those found in the field by Roseboom et al (2012) in a spectroscopic sample of MIPS-and SPIREselected galaxies at redshifts similar to the ones probed in our sample (0.8 < z < 1.8). However, the difference in nebular extinction between the subsamples does not necessarily translate in a straightforward manner to a difference in the extinction of the stellar continuum.…”

Section: Mean Stellar and Starburst Ages As A Function Of Tir Luminositysupporting

confidence: 81%

“…The host galaxies of radio-and IR-selected AGN have also been the subjects of investigation with Herschel (e.g., Hardcastle et al 2012;Del Moro et al 2013), though the connection between these AGNs and their host galaxies is less clear than in the case of X-ray-selected AGN. Additionally, large populations of starbursting galaxies without an active nucleus have been studied with Herschel, resulting in insights into the relationship between stellar mass and the SFR in star-forming galaxies (e.g., Elbaz et al 2011;Rodighiero et al 2011;Hilton et al 2012), specific star formation rates (SSFRs) and dust mass (Smith et al 2012a), various SFR indicators (Wuyts et al 2011;Domínguez Sánchez et al 2012), and a variety of other properties (e.g., Casey 2012;Casey et al 2012a;Roseboom et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Lemaux

Floc’h

Fèvre

et al. 2014

A&A

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We investigate of the properties of ∼2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4 in the CFHTLS-D1 field. Using a combination of extensive spectroscopy from the VVDS and ORELSE surveys, deep multiwavelength imaging from CFHT, VLA, Spitzer, XMM-Newton, and Herschel, and well-calibrated spectral energy distribution fitting, Herschel-bright galaxies are compared to optically-selected galaxies at a variety of redshifts. Herschel-selected galaxies are observed to span a range of stellar masses, colors, and absolute magnitudes equivalent to galaxies undetected in SPIRE. Though many Herschel galaxies appear to be in transition, such galaxies are largely consistent with normal star-forming galaxies when rest-frame colors are utilized. The nature of the star-forming "main sequence" is studied and we warn against adopting this framework unless the main sequence is determined precisely. Herschel galaxies at different total infrared luminosities (L TIR ) are compared. Bluer optical colors, larger nebular extinctions, and larger contributions from younger stellar populations are observed for galaxies with larger L TIR , suggesting that low-L TIR galaxies are undergoing rejuvenated starbursts while galaxies with higher L TIR are forming a larger percentage of their stellar mass. A variety of methods are used to select powerful active galactic nuclei (AGN). Galaxies hosting all types of AGN are observed to be undergoing starbursts more commonly and vigorously than a matched sample of galaxies without powerful AGN and, additionally, the fraction of galaxies with an AGN increases with increasing star formation rate at all redshifts. At all redshifts (0 < z < 4) the most prodigious star-forming galaxies are found to contain the highest fraction of powerful AGN. For redshift bins that allow a comparison (z > 0.5), the highest L TIR galaxies in a given redshift bin are unobserved by SPIRE at subsequently lower redshifts, a trend linked to downsizing. In conjunction with other results, this evidence is used to argue for prevalent AGN-driven quenching in starburst galaxies across cosmic time.

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Section: Mean Stellar and Starburst Ages As A Function Of Tir Luminositysupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Lemaux

Floc’h

Fèvre

et al. 2014

A&A

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“…Since these local IR galaxies show interaction features such as multiple galaxy systems, tidal tails or bridges, and disturbed morphology, the sources are considered as ongoing or pre-mergers. On the other hand, Roseboom et al (2012) investigated 57 Herschel/SPIRE sources at z ∼ 1.2 and concluded that the mass-metallicity relation of their sample is indistinguishable from the local mass-metallicity relation, which is consistent with the results of our IR galaxies at z ∼ 0.88. Results of these studies suggest that there is a discrepancy of behavior of the mass-metallicity relations between IR galaxies at low and high redshift compared with MS galaxies.…”

Section: Comparison With Other Ir Galaxy Samplessupporting

confidence: 85%

“…Luminous and ultra luminous infrared galaxies (LIRGs and ULIRGs) in the local Universe are found to have lower metallicity at a similar stellar mass compared with optically selected star-forming galaxies (Rupke et al 2008;Rodrigues et al 2008;Kilerci Eser et al 2014). On the other hand, a study of metallicity of Herschel selected far-IR galaxies at z > 1 by Roseboom et al (2012) do not show any clear metallicity deficit compared with local optical selected galaxies (see also Silverman et al 2015). That is, there is no general consensus yet.…”

mentioning

confidence: 95%

The mass–metallicity relation of AKARI-FMOS infrared galaxies at z ∼ 0.88 in the AKARI North Ecliptic Pole Deep Survey Field

Oi¹,

Goto²,

Malkan³

et al. 2017

Publications of the Astronomical Society of Japan

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Mass, metallicity, and star formation rate (SFR) of a galaxy are crucial parameters in understanding galaxy formation and evolution. However, the relation among these, (i.e., the fundamental relation) is still a matter of debate for luminous infrared galaxies, which carry a bulk of star formation rate budget of the universe at z∼1. We have investigated the relation among stellar mass, gas-phase oxygen abundance, and SFR of AKARI-detected mid-IR galaxies at z∼ 0.88 in the AKARI NEP deep field. We observed ∼350 AKARI sources with Subaru/FMOS near-infrared spectrograph, and detected sure Hα emission lines from 25 galaxies and ex-1 pected Hα emission lines from 44 galaxies. The SF R Hα,IR of our sample is almost constant ( SF R Hα,IR = ∼ 25 M ⊙ yr −1 ) over the stellar mass range of our sample. Compared with main-sequence (MS) galaxies at a similar redshift range (z ∼ 0.78), the average SFR of our detected sample is comparable for massive galaxies (∼10 10.58 M ⊙ ), while higher by ∼0.6 dex for less massive galaxies (∼10 10.05 M ⊙ ). We measure metallicities from the [N II]/Hα emission line ratio. We find that the mass-metallicity relation of our individually measured sources agrees with that for optical-selected star-forming galaxies at z ∼ 0.1, while metallicities of stacked spectra agree with that of MS galaxies at z ∼ 0.78. Considering high SFR of individually measured sources, fundamental metallicity relation (FMR) of the IR galaxies is different from that at z∼0.1. However, on the mass-metallicity plane, they are consistent with the MS galaxies, highlighting higher SFR of the IR galaxies. This suggests the evolutionary path of our infrared galaxies is different from that of MS galaxies. A possible physical interpretation includes that the star-formation activities of infrared galaxies at z ∼ 0.88 in our sample are enhanced by interaction and/or merger of galaxies, but the inflow of metal-poor gas is not yet induced, keeping the metallicity intact.

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“…3. Source photometry to measure source photometry using a modified De-blended SPIRE Photometry algorithm (Roseboom et al 2010(Roseboom et al , 2012.…”

Section: Fir/sub-mm Photometrymentioning

confidence: 99%

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

2016

ApJ

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In this work, we present a study of 207 quasars selected from the Sloan Digital Sky Survey quasar catalogs and the Herschel Stripe 82 survey. Quasars within this sample are high-luminosity quasars with a mean bolometric luminosity of 10 46.4 erg s −1 . The redshift range of this sample is within z < 4, with a mean value of 1.5 ± 0.78. Because we only selected quasars that have been detected in all three Herschel-SPIRE bands, the quasar sample is complete yet highly biased. Based on the multi-wavelength photometric observation data, we conducted a spectral energy distribution (SED) fitting through UV to FIR. Parameters such as active galactic nucleus (AGN) luminosity, far-IR (FIR) luminosity, stellar mass, as well as many other AGN and galaxy properties are deduced from the SED fitting results. The mean star formation rate (SFR) of the sample is 419 M e yr −1 and the mean gas mass is ∼10 11.3 M e . All of these results point to an IR luminous quasar system. Compared with star formation main sequence (MS) galaxies, at least 80 out of 207 quasars are hosted by starburst galaxies. This supports the statement that luminous AGNs are more likely to be associated with major mergers. The SFR increases with the redshift up to z = 2. It is correlated with the AGN bolometric luminosity, where µ  L L FIR Bol 0.46 0.03 . The AGN bolometric luminosity is also correlated with the host galaxy mass and gas mass. Yet the correlation between L FIR and L Bol has higher significant level, implies that the link between AGN accretion and the SFR is more primal. The M BH /M * ratio of our sample is 0.02, higher than the value 0.005 in the local universe. It might indicate an evolutionary trend of the M BH -M * scaling relation.

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FMOS near-IR spectroscopy ofHerschel-selected galaxies: star formation rates, metallicity and dust attenuation atz∼ 1

Cited by 38 publications

References 80 publications

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

The mass–metallicity relation of AKARI-FMOS infrared galaxies at z ∼ 0.88 in the AKARI North Ecliptic Pole Deep Survey Field

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

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