Rest‐Frame Optical Spectroscopic Classifications for Submillimeter Galaxies

Takata, Tadafumi; Sekiguchi, K.; Smail, Ian; Chapman, Scott; Swinbank, A. M.; Blain, A. W.; Ivison, R. J.

doi:10.1086/507985

Cited by 79 publications

(139 citation statements)

References 87 publications

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“…The sub-millimetre and radio fluxes of this population of galaxies indicate that their bolometric luminosities are comparable to local ULIRGs, whereas their mid-IR emission seems to be similar to the observed in local LIRGs (Kovács et al 2006;Takata et al 2006;Menéndez-Delmestre et al 2009). Besides this, recent IFS-based observations of SMGs reveal that they present evidence of clumpy star formation on kiloparsec scales and similar star-formation rate surface densities (Σ SFR ) to the local counterparts (Nesvadba et al 2007;Harrison et al 2012;Alaghband-Zadeh et al 2012;Menéndez-Delmestre et al 2013).…”

Section: Implication For Extinction-corrected Properties In High-z Gasupporting

confidence: 51%

“…HST-NICMOS and ACS observations reflect structured dust obscuration in these objects (Swinbank et al 2010). In particular, Takata et al (2006) find that the internal extinction in these objects are similar to the extinction in local ULIRGs, and measured a median extinction of A V = 2.9 ± 0.5 mag in a sample of SMGs at z ∼ 1.0-3.5 using the H α /H β flux ratio. Clumpy and dusty star-forming structures have also been identified at high redshifts in more common star forming galaxies (i.e.…”

Section: Implication For Extinction-corrected Properties In High-z Gamentioning

confidence: 69%

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VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2013

A&A

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We present a 2D study of the internal extinction on (sub)kiloparsec scales of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7), based on near-infrared Paα, Brδ, and Brγ line ratios, obtained with VLT-SINFONI integral-field spectroscopy (IFS). The 2D extinction (A V ) distributions of the objects, map regions of ∼3 × 3 kpc (LIRGs) and ∼12 × 12 kpc (ULIRGs), with average angular resolutions (FWHM) of ∼0.2 kpc and ∼0.9 kpc, respectively. The individual A V galaxy distributions indicate a very clumpy dust structure already on sub-kiloparsec scales, with values (per spaxel) ranging from A V ∼ 1 to 20 mag in LIRGs, and from A V ∼ 2 to 15 mag in ULIRGs. As a class, the median values of the distributions are A V = 5.3 mag and A V = 6.5 mag for the LIRG and ULIRG subsamples, respectively. In ∼70% of the objects, the extinction peaks at the nucleus with values ranging from A V ∼ 3 to 17 mag. Within each galaxy, the A V radial profile shows a mild decrement in LIRGs within the inner 2 kpc radius, while the same radial variation is not detected in ULIRGs, likely because of the lower linear scale resolution of the observations at the distance of ULIRGs. We evaluated the effects of the galaxy distance in the measurements of the extinction as a function of the linear scale (in kpc) of the spaxel (i.e. due to the limited angular resolution of the observations). If the distribution of the gas/dust and star-forming regions in local LIRGs (63 Mpc, 40 pc/spaxel on average) is the same for galaxies at greater distances, the observed median A V values based on emission line ratios would be a factor ∼0.8 lower at the average distance of our ULIRG sample (328 Mpc, 0.2 kpc/spaxel), and a factor ∼0.67 for galaxies located at distances of more than 800 Mpc (0.4 kpc/spaxel). This distance effect would have implications for deriving the intrinsic extinction in high-z star-forming galaxies and for subsequent properties such as star formation rate, star formation surface density, and KS-law, based on Hα line fluxes. If local LIRGs are analogues of the main-sequence star-forming galaxies at cosmological distances, the extinction values (A V ) derived from the observed emission lines in these high-z sources would need to be increased by a factor 1.4 on average.

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Section: Implication For Extinction-corrected Properties In High-z Gasupporting

confidence: 51%

Section: Implication For Extinction-corrected Properties In High-z Gamentioning

confidence: 69%

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2013

A&A

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“…(1) originally taken from Goldsmith et al (2012) to derive a C + column density, N(C + ) = 1.4 × 10 17 τdv[cm −2 ], we find N(C + ) = 8.2 × 10 18 cm −2 , corresponding to N(HI) = 5.9 × 10 22 cm −2 when adopting the Galactic carbon abundance of 1.4 × 10 −4 . This choice is reasonable for massive dusty starburst galaxies at high redshift, which have gas-phase metallicities comparable to those in the Milky Way (Takata et al 2006;Nesvadba et al 2007), but might be too high for infall of more pristine gas. For solar metallicity, this column density is about a factor of 2 higher than the most extreme values found in the Milky Way, and is accordingly more suitable for lower metallicity gas.…”

Section: Astrophysical Nature Of [Cii] In the Garnetmentioning

confidence: 99%

Planck’s Dusty GEMS

Nesvadba

Kneißl

Cañameras

et al. 2016

A&A

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We present spatially resolved ALMA [CII] observations of the bright (flux density S 350 = 400 mJy at 350 µm), gravitationally lensed, starburst galaxy PLCK G045.1+61.1 at z = 3.427, the "Garnet". This source is part of our set of "Planck's Dusty GEMS", discovered with the Planck's all-sky survey. Two emission-line clouds with a relative velocity offset of ∼600 km s −1 extend towards north-east and south-west, respectively, of a small, intensely star-forming clump with a star-formation intensity of 220 M yr −1 kpc −2 , akin to maximal starbursts.[CII] is also seen in absorption, with a redshift of +350 km s −1 relative to the brightest CO component.[CII] absorption has previously only been found in the Milky Way along sightlines toward bright high-mass star-forming regions, and this is the first detection in another galaxy. Similar to Galactic environments, the [CII] absorption feature is associated with [CI] emission, implying that this is diffuse gas shielded from the UV radiation of the clump, and likely at large distances from the clump. Since absorption can only be seen in front of a continuum source, the gas in this structure can definitely be attributed to gas flowing towards the clump. The absorber could be part of a cosmic filament or merger debris being accreted onto the galaxy. We discuss our results also in light of the on-going debate of the origin of the [CII] deficit in dusty star-forming galaxies.

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“…Due to the coarse resolution of SCUBA, localizations derived from high-resolution radio maps had to be used to measure their spectroscopic redshifts . Lots of studies have addressed the issue of characterizing the nature of SMGs (Egami et al 2004;Greve et al 2004Greve et al , 2005Smail et al 2004;Swinbank et al 2004Swinbank et al , 2006Swinbank et al , 2008Takagi et al 2004;Alexander et al 2005;Borys et al 2005;Kovács et al 2006;Laurent et al 2006;Pope et al 2006;Tacconi et al 2006Tacconi et al , 2008Takata et al 2006;Younger et al 2007Younger et al , 2008Younger et al , 2009aClements et al 2008;Coppin et al 2008;Dye et al 2008Dye et al , 2009Hainline et al 2009;Perera et al 2008;Scott et al 2008;Austermann et al 2009;Devlin et al 2009;Eales et al 2009;Murphy et al 2009;Murphy 2009;Tamura et al 2009;Weiß et al 2009b;Aravena et al 2010, some of these works were based on surveys with sensitivity worse than 3 mJy quoted above). However they were usually based on limited samples ( 20 sources), limited wavelength coverage or photometric redshifts.…”

Section: Introductionmentioning

confidence: 99%

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Michalowski

Hjorth

Watson

2010

A&A

234

278

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The nature of galaxies selected at submillimeter wavelengths (SMGs, S 850 3 mJy), some of the bolometrically most luminous objects at high redshifts, is still elusive. In particular their star formation histories and source of emission are not accurately constrained. In this paper we introduce a new approach to analyse the SMG data. Namely, we present the first self-consistent UV-to-radio spectral energy distribution fits of 76 SMGs with spectroscopic redshifts using all photometric datapoints from ultraviolet to radio simultaneously. We find that they are highly star-forming (median star formation rate 713 M yr −1 for SMGs at z > 0.5), moderately dust-obscured (median A V ∼ 2 mag), hosting significant stellar populations (median stellar mass 3.7 × 10 11 M ) of which only a minor part has been formed in the ongoing starburst episode. This implies that in the past, SMGs experienced either another starburst episode or merger with several galaxies. The properties of SMGs suggest that they are progenitors of present-day elliptical galaxies. We find that these bright SMGs contribute significantly to the cosmic star formation rate density (∼20%) and stellar mass density (∼30-50%) at redshifts 2-4. Using number counts at low fluxes we find that as much as 80% of the cosmic star formation at these redshifts took place in SMGs brighter than 0.1 mJy. We find evidence that a linear infrared-radio correlation holds for SMGs in an unchanged form up to redshift of 3.6, though its normalization is offset from the local relation by a factor of ∼2.1 towards higher radio luminosities. We present a compilation of photometry data of SMGs and determinations of cosmic SFR and stellar mass densities.

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Rest‐Frame Optical Spectroscopic Classifications for Submillimeter Galaxies

Cited by 79 publications

References 87 publications

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

Planck’s Dusty GEMS

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

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