Should we believe the results of ultraviolet–millimetre galaxy spectral energy distribution modelling?

Hayward, Christopher C.; Smith, D. J. B.

doi:10.1093/mnras/stu2195

Cited by 100 publications

(96 citation statements)

References 174 publications

(246 reference statements)

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“…This may indicate a hidden, radio emitting AGN, but from our SED analysis in Section 4, we have shown that if HLock01-R harbors an AGN, its contribution to the total L IR and SFR is modest (;1%), as also noted by Rigopoulou et al (2018), and even assuming a maximum of 20% of an AGN contribution to the IRAC fluxes, the stellar mass of HLock01-R will be lower only by 0.1 dex, which is within our measurement errors. Moreover, Hayward & Smith (2015) have also shown that the physical properties derived using MAGPHYS are robust even when the AGN contributes 25% of the total UV to IR luminosity. Our deep GTC/OSIRIS rest-frame UV spectroscopy does not show any line or continuum emission at the positions of the lensed 13 images of HLock01-R, as some of them are included in the regions covered by our long-slit spectra (see Figure 1, left panel).…”

Section: Physical Propertiesmentioning

confidence: 95%

The Strong Gravitationally Lensed Herschel Galaxy HLock01: Optical Spectroscopy Reveals a Close Galaxy Merger with Evidence of Inflowing Gas

Marques-Chaves

Pérez-Fournón

Gavazzi

et al. 2018

ApJ

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Citation for published item:w rquesEgh vesD ui nd ¡ erezEpournonD ssm el nd q v zziD ph el nd w rt¡ %nezEx v j sD lom sF nd ie hersD hominik nd igopoulouD himitr nd g rer Ev versD entonio nd glementsD h vid vF nd goor yD es nth nd p rr hD hun n nd svisonD o tF nd tim¡ enezE ¡ engelD g milo iF nd x yyeriD roosh ng nd yliverD e nd ymontD el in nd ottD hougl s nd huD iping nd rdlowD tulie @PHIVA 9 he strong gr vit tion lly lensed rers hel q l xy rvo kHI X opti l spe tros opy reve ls lose g l xy merger with eviden e of in)owing g sF9D estrophysi l journ lFD VSR @PAF pF ISIF Further information on publisher's website: Additional information:Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractThe submillimeter galaxy (SMG) HERMES J105751.1+573027 (hereafter HLock01) at z=2.9574±0.0001 is one of the brightest gravitationally lensed sources discovered in the Herschel Multi-tiered Extragalactic Survey. Apart from the high flux densities in the far-infrared, it is also extremely bright in the rest-frame ultraviolet (UV), with a total apparent magnitude m UV ;19.7 mag. We report here deep spectroscopic observations with the Gran Telescopio Canarias of the optically bright lensed images of HLock01. Our results suggest that HLock01 is a merger system composed of the Herschel-selected SMG and an optically bright Lyman break-like galaxy (LBG), separated by only 3.3 kpc in projection. While the SMG appears very massive(M * ;5×10 11 M e ), with a highly extinguished stellar component (A V ;4.3 ), the LBG is a young, lower-mass (M * ;1×10 10 M e ), but still luminous ( L 10 UV * ) satellite galaxy. Detailed analysis of the high signal-to-noise ratio (S/N) rest-frame UV spectrum of the LBG shows complex kinematics of the gas, exhibiting both blueshifted and redshifted absorption components. While the blueshifted component is associated with strong galactic outflows from the massive stars in the LBG, as is common in most star-forming galaxies, the redshifted component may be associated with gas inflow seen along a favorable sightline to the LBG. We also find evidence of an extended gas reservoir around HLock01 at an impact parameter of 110 kpc, through the detection of C II λλ1334 absorption in the red wing of a bright Lyα emitter at z;3.327. The data presented here highlight the power of gravitational lensing in high S/N studies to probe deeply into the physics of high-z star-forming galaxies.

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Section: Physical Propertiesmentioning

confidence: 95%

The Strong Gravitationally Lensed Herschel Galaxy HLock01: Optical Spectroscopy Reveals a Close Galaxy Merger with Evidence of Inflowing Gas

Marques-Chaves

Pérez-Fournón

Gavazzi

et al. 2018

ApJ

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“…This code has been tested on simulated isolated galaxies and major mergers and has been shown to correctly retrieve   , SFRs, and L IR of the simulated objects (Hayward & Smith 2015). It was also shown in da Cunha et al (2013) that MAGPHYS, when used to fit U−K photometry, can accurately predict the L IR derived for the same galaxies from Herschel measurements.…”

Section: Sfrs Stellar Masses and Sizesmentioning

confidence: 96%

Deep CO(1–0) Observations of z = 1.62 Cluster Galaxies with Substantial Molecular Gas Reservoirs and Normal Star Formation Efficiencies

Rudnick

Hodge

Walter

et al. 2017

ApJ

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We present an extremely deep CO(1-0) observation of a confirmed z = 1.62 galaxy cluster. We detect two spectroscopically confirmed cluster members in CO(1-0) with signal-to-noise ratio >5. Both galaxies have log (  /  ) > 11 and are gas rich, with  mol /(  + mol )∼0.17-0.45. One of these galaxies lies on the star formation rate (SFR)-  sequence, while the other lies an order of magnitude below. We compare the cluster galaxies to other SFR-selected galaxies with CO measurements and find that they have CO luminosities consistent with expectations given their infrared luminosities. We also find that they have gas fractions and star formation efficiencies (SFE) comparable to what is expected from published field galaxy scaling relations. The galaxies are compact in their stellar light distribution, at the extreme end for all high-redshift star-forming galaxies. However, their SFE is consistent with other field galaxies at comparable compactness. This is similar to two other sources selected in a blind CO survey of the HDF-N. Despite living in a highly quenched protocluster core, the molecular gas properties of these two galaxies, one of which may be in the process of quenching, appear entirely consistent with field scaling relations between the molecular gas content, stellar mass, star formation rate, and redshift. We speculate that these cluster galaxies cannot have any further substantive gas accretion if they are to become members of the dominant passive population in < z 1 clusters.

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“…To date, there are still a few studies that explore and quantify the impact of AGN contamination on the determination of the underlying host galaxy properties via SED-fitting (Wuyts et al 2011;Hayward & Smith 2015). In this paper, we address this using the Bayesian-based SED-fitting code CIGALE (Noll et al 2009, Burgarella et al, in prep.…”

Section: Introductionmentioning

confidence: 99%

Constraining the properties of AGN host galaxies with spectral energy distribution modelling

Ciesla

Charmandaris

Georgakakis

et al. 2015

A&A

233

354

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Detailed studies of the spectral energy distribution (SED) of normal galaxies have increasingly been used to understand the physical mechanism dominating their integrated emission, mainly owing to the availability of high quality multi-wavelength data from the UV to the far-infrared (FIR). However, systems hosting dust-enshrouded nuclear starbursts and/or an accreting supermassive black hole (an active galactic nucleus or AGN) are especially challenging to study. This is due to the complex interplay between the heating by massive stars and the AGN, the absorption and emission of radiation from dust, as well as the presence of the underlying old stellar population. We used the latest release of CIGALE, a fast state-of-the-art galaxy SED-fitting model relying on energy balance, to study the influence of an AGN in a self consistent manner in estimating both the star formation rate (SFR) and stellar mass in galaxies, as well as to calculate the contribution of the AGN to the power output of the host. Using the semi-analytical galaxy formation model , we created a suite of mock galaxy SEDs using realistic star formation histories (SFH). We also added an AGN of Type-1, Type-2, or intermediate-type whose contribution to the bolometric luminosity can be variable. We performed an SED-fitting of these catalogues with CIGALE, assuming three different SFHs: a single-exponentially-decreasing (1τ-dec), a double-exponentiallydecreasing (2τ-dec), and a delayed SFH. Constraining the overall contribution of an AGN to the total infrared luminosity (frac AGN ) is very challenging for frac AGN < 20%, with uncertainties of ∼5-30% for higher fractions depending on the AGN type, while FIR and sub-mm are essential. The AGN power has an impact on the estimation of M * in Type-1 and intermediate-type AGNs but has no effect on galaxies hosting Type-2 AGNs. We find that in the absence of AGN emission, the best estimates of M * are obtained using the 2τ-dec model but at the expense of realistic ages of the stellar population. The delayed SFH model provides good estimates of M * and SFR, with a maximum offset of 10% as well as better estimates of the age. Our analysis shows that the under-estimation of the SFR increases with frac AGN for Type-1 systems, as well as for low contributions of an intermediate AGN type, but it is quite insensitive to the emission of Type-2 AGNs up to frac AGN ∼ 45%. A lack of sampling the FIR, or sub-mm domain systematically over-estimates the SFR (<20%), independent of the contribution of the AGN. Similarly, the UV emission is critical in accurately retrieving both the M * for Type-1 and intermediate-type AGN and the SFR of all three AGN types. We show that the presence of AGN emission introduces a scatter to the SFR-M * main sequence relation derived from SED-fitting, which is driven by the uncertainties on M * . Finally, we used our mock catalogues to test the popular IR SED-fitting code DIR and show that frac AGN is under-estimated but that the SFR is recovered well for Type-1 and intermedia...

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Should we believe the results of ultraviolet–millimetre galaxy spectral energy distribution modelling?

Cited by 100 publications

References 174 publications

The Strong Gravitationally Lensed Herschel Galaxy HLock01: Optical Spectroscopy Reveals a Close Galaxy Merger with Evidence of Inflowing Gas

The Strong Gravitationally Lensed Herschel Galaxy HLock01: Optical Spectroscopy Reveals a Close Galaxy Merger with Evidence of Inflowing Gas

Deep CO(1–0) Observations of z = 1.62 Cluster Galaxies with Substantial Molecular Gas Reservoirs and Normal Star Formation Efficiencies

Constraining the properties of AGN host galaxies with spectral energy distribution modelling

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