A bright<i>z</i>= 5.2 lensed submillimeter galaxy in the field of Abell 773

Combes, F.; Rex, M.; Rawle, Tim; Egami, Eiichi; Boone, F.; Smail, Ian; Richard, Johan; Ivison, R. J.; Gurwell, M. A.; Casey, Caitlin M.; Omont, A.; Alba, A. Berciano; Dessauges‐Zavadsky, M.; Edge, A. C.; Fazio, G. G.; Kneib, Jean-Paul; Okabe, Nobuhiko; Pelló, R.; Pérez‐González, Pablo G.; Schaerer, D.; Smith, Graham P.; Swinbank, A. M.; Werf, P. van der

doi:10.1051/0004-6361/201118750

Cited by 140 publications

(182 citation statements)

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“…Combes et al (2011Combes et al ( , 2012Combes et al ( , 2013, Danielson et al (2011), Fu et al (2012, Sharon et al (2013), Rawle et al (2014), and Magdis et al (2014).…”

Section: Comparison Samplementioning

confidence: 99%

Molecular gas content in strongly lensedz~ 1.5−3 star-forming galaxies with low infrared luminosities

Dessauges‐Zavadsky

Zamojski

Schaerer

et al. 2015

A&A

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To extend the molecular gas measurements to more typical star-forming galaxies (SFGs) with star formation rates SFR < 40 M yr −1 and stellar masses M * < 2.5 × 10 10 M at z ∼ 1.5−3, we have observed CO emission with the IRAM Plateau de Bure Interferometer and the IRAM 30 m telescope for five strongly lensed galaxies, selected from the Herschel Lensing Survey. These observations are combined with a compilation of CO measurements from the literature. From this, we infer the CO luminosity correction factors r 2,1 = 0.81 ± 0.20 and r 3,1 = 0.57 ± 0.15 for the J = 2 and J = 3 CO transitions, respectively, valid for SFGs at z > 1. The combined sample of CO-detected SFGs at z > 1 shows a large spread in star formation efficiency (SFE) with a dispersion of 0.33 dex, such that the SFE extends well beyond the low values of local spirals and overlaps the distribution of z > 1 submm galaxies. We find that the spread in SFE (or equivalently in molecular gas depletion timescale) is due to the variations of several physical parameters, primarily the specific star formation rate, and also stellar mass and redshift. The dependence of SFE on the offset from the main sequence and the compactness of the starburst is less clear. The possible increase of the molecular gas depletion timescale with stellar mass, now revealed by low M * SFGs at z > 1 and also observed at z = 0, contrasts with the generally acknowledged constant molecular gas depletion timescale and refutes the linearity of the Kennicutt-Schmidt relation. A net rise of the molecular gas fraction ( f gas ) is observed from z ∼ 0.2 to z ∼ 1.2, followed by a very mild increase toward higher redshifts, as found in earlier studies. At each redshift the molecular gas fraction shows a large dispersion, mainly due to the dependence of f gas on stellar mass, producing a gradient of increasing f gas with decreasing M * . We provide the first measurement of the molecular gas fraction of z > 1 SFGs at the low-M * end between 10 9.4 < M * /M < 10 9.9 , reaching a mean f gas = 0.69 ± 0.18, which shows a clear f gas upturn at these lower stellar masses. Finally, we find evidence for a nonuniversal dust-to-gas ratio among high-redshift SFGs, high-redshift submm galaxies, local spirals, and local ultraluminous IR galaxies with near-solar metallicities, as inferred from a homogeneous analysis of their rest-frame 850 μm luminosity per unit gas mass. The SFGs with z > 1 show a trend for a lower L ν (850 μm)/M gas mean by 0.33 dex compared to the other galaxy populations.

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“…Combes et al (2011Combes et al ( , 2012Combes et al ( , 2013, Danielson et al (2011), Fu et al (2012, Sharon et al (2013), Rawle et al (2014), and Magdis et al (2014).…”

Section: Comparison Samplementioning

confidence: 99%

Molecular gas content in strongly lensedz~ 1.5−3 star-forming galaxies with low infrared luminosities

Dessauges‐Zavadsky

Zamojski

Schaerer

et al. 2015

A&A

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“…This is consistent with our earlier study on LESS J0332 (De Breuck et al 2011), where we estimated that the XDR contribution to the [C ii] 158 μm is ∼1.3%, based on the absorption-corrected X-ray luminosity of L 2−10 keV = 2.5 × 10 44 erg s −1 (Gilli et al 2011) and a scaling relation of L [CII],AGN = 2 × 10 −3 L 2−10 keV (Stacey et al 2010). At high-z [N ii] 205 μm has been detected in HLS J091828.6+514223 at z = 5.24 (Combes et al 2012), APM 08279+5255 at z = 3.91, and MM 18423+5938 at z = 3.93 (Decarli et al 2012). However, their [C ii] 158 μm line has not been observed and consequently their [N ii]/[C ii] ratio is unknown (see Walter et al 2009b, and references therein).…”

Section: Possible Agn Contributionmentioning

confidence: 99%

“…Since the volume ratio of H ii regions and PDRs also depends on cloud properties such as the gas density and ionization structure (hence the ionization parameter), the observed [N ii]/[C ii] flux ratio accordingly depends on those parameters. Recently, [N ii] 205 μm detections have been obtained for three strongly lensed galaxies at z ∼ 4−5 (Decarli et al 2012;Combes et al 2012); however a [C ii] 158 μm detection has not been reported in any of these galaxies.…”

Section: Introductionmentioning

confidence: 99%

ALMA reveals a chemically evolved submillimeter galaxy atz= 4.76

Nagao

Maiolino

Breuck

et al. 2012

A&A

101

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The chemical properties of high-z galaxies provide important information for constraining galaxy evolutionary scenarios. However, widely used metallicity diagnostics based on rest-frame optical emission lines are unusable for heavily dust-enshrouded galaxies (such as submillimeter galaxies; SMGs), especially at z > 3. Here we focus on the flux ratio of the far-infrared fine-structure emis- .008. This is the first measurement of the [N ii]/[C ii]flux ratio in high-z galaxies, and the inferred flux ratio is similar to the ratio observed in the nearby universe (∼0.02−0.07). The velocity-integrated flux ratio and photoionization models suggest that the metallicity in this SMG is consistent with solar, implying that the chemical evolution has progressed very rapidly in this system at z = 4.76. We also obtain a tight upper limit on the CO(12−11) transition, which translates into CO(12−11)/CO(2−1) < 3.8 (3σ). This suggests that the molecular gas clouds in LESS J033229.4-275619 are not significantly affected by the radiation field emitted by the AGN in this system.

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“…Not much is observationally known about the CO excitation properties of indisputably normal MS galaxies at high redshift. The most detailed information is available for IR-luminous systems selected either as submillimeter galaxies (SMGs; e.g., Bothwell et al 2013;Riechers et al 2013) or strong lenses (Danielson et al 2011;Cox et al 2011;Combes et al 2012;Scott et al 2011;Spilker et al 2014). In a pilot study, Dannerbauer et al (2009) presented CO[3-2] observations of one z = 1.5 galaxy (BzK-21000, further discussed in this paper) that was previously detected in CO[2-1], finding a low CO[3-2]/CO[2-1] ratio fairly consistent with the Milky Way (MW).…”

Section: Introductionmentioning

confidence: 99%

CO excitation of normal star-forming galaxies out toz= 1.5 as regulated by the properties of their interstellar medium

Daddi

Dannerbauer

Liu

et al. 2015

A&A

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We investigate the CO excitation of normal (near-IR selected BzK) star-forming (SF) disk galaxies at z = 1.5 using IRAM Plateau de Bure observations of the CO[2-1], CO , and CO[5-4] transitions for four galaxies, including VLA observations of CO[1-0] for three of them, with the aim of constraining the average state of H 2 gas. By exploiting previous knowledge of the velocity range, spatial extent, and size of the CO emission, we measure reliable line fluxes with a signal-to-noise ratio >4-7 for individual transitions. While the average CO spectral line energy distribution (SLED) has a subthermal excitation similar to the Milky Way (MW) up to CO[3-2], we show that the average CO emission is four times stronger than assuming MW excitation. This demonstrates that there is an additional component of more excited, denser, and possibly warmer molecular gas. The ratio of CO[5-4] to lower-J CO emission is lower than in local (ultra-)luminous infrared galaxies (ULIRGs) and high-redshift starbursting submillimeter galaxies, however, and appears to be closely correlated with the average intensity of the radiation field U and with the star formation surface density, but not with the star formation efficiency. The luminosity of the CO transition is found to be linearly correlated with the bolometric infrared luminosity over four orders of magnitudes. For this transition, z = 1.5 BzK galaxies follow the same linear trend as local spirals and (U)LIRGs and high-redshift star-bursting submillimeter galaxies. The CO[5-4] luminosity is thus empirically related to the dense gas and might be a more convenient way to probe it than standard high-density tracers that are much fainter than CO. We see excitation variations among our sample galaxies that can be linked to their evolutionary state and clumpiness in optical rest-frame images. In one galaxy we see spatially resolved excitation variations, where the more highly excited part of the galaxy corresponds to the location of massive SF clumps. This provides support to models that suggest that giant clumps are the main source of the high-excitation CO emission in high-redshift disk-like galaxies.

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A brightz= 5.2 lensed submillimeter galaxy in the field of Abell 773

Cited by 140 publications

References 50 publications

Molecular gas content in strongly lensedz~ 1.5−3 star-forming galaxies with low infrared luminosities

Molecular gas content in strongly lensedz~ 1.5−3 star-forming galaxies with low infrared luminosities

ALMA reveals a chemically evolved submillimeter galaxy atz= 4.76

CO excitation of normal star-forming galaxies out toz= 1.5 as regulated by the properties of their interstellar medium

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