A multiwavelength consensus on the main sequence of star-forming galaxies at z ∼ 2

Rodighiero, G.; Renzini, A.; Daddi, E.; Baronchelli, Ivano; Berta, S.; Cresci, G.; Franceschini, A.; Gruppioni, C.; Lutz, D.; Mancini, C.; Santini, P.; Zamorani, G.; Silverman, John D.; Kashino, Daichi; Andreani, P.; Cimatti, A.; Sánchez, H. Domínguez; Floc’h, E. Le; Magnelli, B.; Popesso, P.; Pozzi, F.

doi:10.1093/mnras/stu1110

Cited by 129 publications

(151 citation statements)

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“…Another population, which is likely missed by VUDS, are galaxies that are heavily starforming but strongly obscured by dust. As shown by Rodighiero et al (2014) and Whitaker et al (2012) comparing UV-selected and IR-selected samples, we expect to have missed less than 7% of high-mass high-SFR galaxies lying mostly above the MS. This fraction of possibly missed galaxies is not high enough to produce the trend we observe in our data.…”

Section: A Turn-off In the Sfr-m Relation: Evolution With Redshiftmentioning

confidence: 85%

“…At higher redshifts z > 2 the sensitivity of Herschel has enabled the infrared luminosity (L IR ) to be measured on samples of a few hundred galaxies (e.g. Lemaux et al 2014;Rodighiero et al 2014). Measuring M and SFR is most often performed by the same process along with photometric redshift determination because z phot , M , and SFR may all rely on the same template fitting of the observed photometry distribution over a broad wavelength range.…”

Section: Introductionmentioning

confidence: 99%

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The evolving star formation rate:M_⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey

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Hathi

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We study the evolution of the star formation rate (SFR) -stellar mass (M ) relation and specific star formation rate (sSFR) of star-forming galaxies (SFGs) since a redshift z 5.5 using 2435 (4531) galaxies with highly reliable spectroscopic redshifts in the VIMOS Ultra-Deep Survey (VUDS). It is the first time that these relations can be followed over such a large redshift range from a single homogeneously selected sample of galaxies with spectroscopic redshifts. The log(SFR) − log(M ) relation for SFGs remains roughly linear all the way up to z = 5, but the SFR steadily increases at fixed mass with increasing redshift. We find that for stellar masses M ≥ 3.2 × 10 9 M the SFR increases by a factor of ∼13 between z = 0.4 and z = 2.3. We extend this relation up to z = 5, finding an additional increase in SFR by a factor of 1.7 from z = 2.3 to z = 4.8 for masses M ≥ 10 10 M . We observe a turn-off in the SFR-M relation at the highest mass end up to a redshift z ∼ 3.5. We interpret this turn-off as the signature of a strong on-going quenching mechanism and rapid mass growth. The sSFR increases strongly up to z ∼ 2, but it grows much less rapidly in 2 < z < 5. We find that the shape of the sSFR evolution is not well reproduced by cold gas accretion-driven models or the latest hydrodynamical models. Below z ∼ 2 these models have a flatter evolution (1 + z) Φ with Φ = 2−2.25 compared to the data which evolves more rapidly with Φ = 2.8 ± 0.2. Above z ∼ 2, the reverse is happening with the data evolving more slowly with Φ = 1.2 ± 0.1. The observed sSFR evolution over a large redshift range 0 < z < 5 and our finding of a non-linear main sequence at high mass both indicate that the evolution of SFR and M is not solely driven by gas accretion. The results presented in this paper emphasize the need to invoke a more complex mix of physical processes including major and minor merging to further understand the co-evolution of the SFR and stellar mass growth.

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Section: A Turn-off In the Sfr-m Relation: Evolution With Redshiftmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

The evolving star formation rate:M_⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey

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Hathi

et al. 2015

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“…Our objects occupy the upper part of the MS of "normal" star-forming galaxies at z ∼ 1, due to the adopted far-IR selection (corresponding to a selection in SFR, cf. Rodighiero et al 2014). Only one galaxy lies 4×above the MS, so in the starburst region (Rodighiero et al 2011).…”

Section: The Final Samplementioning

confidence: 99%

Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

Puglisi

Rodighiero

Franceschini

et al. 2016

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We combined the spectroscopic information from the 3D-HST survey with Herschel data to characterize the Hα dust attenuation properties of a sample of 79 main sequence star-forming galaxies at z ∼ 1 in the GOODS-S field. The sample was selected in the far-IR at λ = 100 and/or 160 µm and only includes galaxies with a secure Hα detection (S/N > 3). From the low resolution 3D-HST spectra we measured the redshifts and the Hα fluxes for the whole sample. (A factor of 1/1.2 was applied to the observed fluxes to remove the [NII] contamination.) The stellar masses (M ), infrared (L IR ), and UV luminosities (L UV ) were derived from the spectral energy distributions by fitting multiband data from GALEX near-UV to SPIRE 500 µm. We estimated the continuum extinction E star (B − V) from both the IRX = L IR /L UV ratio and the UV-slope, β, and found excellent agreement between the two. The nebular extinction was estimated from comparison of the observed SFR Hα and SFR UV . We obtained f = E star (B − V)/E neb (B − V) = 0.93 ± 0.06, which is higher than the canonical value of f = 0.44 measured in the local Universe. Our derived dust correction produces good agreement between the Hα and IR+UV SFRs for galaxies with SFR > ∼ 20 M /yr and M > ∼ 5 × 10 10 M , while objects with lower SFR and M seem to require a smaller f -factor (i.e. higher Hα extinction correction). Our results then imply that the nebular extinction for our sample is comparable to extinction in the optical-UV continuum and suggest that the f -factor is a function of both M and SFR, in agreement with previous studies.

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“…This is the so-called main-sequence (MS) paradigm, in which starforming galaxies define a tight correlation between their stellar mass and SFR with a dispersion typically of a factor of two (Noeske et al 2007;Elbaz et al 2007Elbaz et al , 2011Daddi et al 2007Daddi et al , 2009aPannella et al 2009;Karim et al 2011;Whitaker et al 2012Whitaker et al , 2014Magdis et al 2010;Rodighiero et al 2011Rodighiero et al , 2014Schreiber et al 2015). When studying the most luminous systems (e.g., selected by means of their ultra-high infrared A&A 577, A46 (2015) bolometric luminosity − L IR (8−1000 μm), beyond 10 12 L at z = 0 or beyond 10 13 L at z = 2; Sargent et al 2012), a rarer kind of galaxy with more extreme sSFR is most often found that likely is in a short-lived, possibly merging-driven, starburst phase.…”

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

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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 multiwavelength consensus on the main sequence of star-forming galaxies at z ∼ 2

Cited by 129 publications

References 45 publications

The evolving star formation rate:M_⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey

The evolving star formation rate:M_⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey

Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

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

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A multiwavelength consensus on the main sequence of star-forming galaxies at z ∼ 2

Cited by 129 publications

References 45 publications

The evolving star formation rate:M⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey

The evolving star formation rate:M⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey

Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

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

Contact Info

Product

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The evolving star formation rate:M_⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey

The evolving star formation rate:M_⋆relation and sSFR sincez≃ 5 from the VUDS spectroscopic survey