Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer<sup>∗</sup>

Wilson, Derek; Cooray, Asantha; Nayyeri, Hooshang; Bonato, M.; Bradford, C. M.; Clements, D. L.; Zotti, G. de; Díaz-Santos, T.; Farrah, D.; Magdis, G.; Michałowski, M. J.; Pearson, Chris; Rigopoulou, D.; Valtchanov, I.; Wang, Lingyu; Wardlow, J. L.

doi:10.3847/1538-4357/aa8cc7

Cited by 17 publications

(12 citation statements)

References 226 publications

(280 reference statements)

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“…However, this line has not been detected at any redshift so far and the condition required to emit such a line would mean we would observe other lines in the full frequency range. The closest observed waterline transition is the H 2 O 3 2,1 − 3 1,2 (at ν rest = 1162.911 GHz detected by Wilson et al 2017). However, this corresponds to a ∼ 2500 km s −1 blueshift, which appears to be very unlikely.…”

Section: The Complex Case Of Gleam 0917mentioning

confidence: 84%

The GLEAMing of the first supermassive black holes

Drouart

Seymour

Galvin

et al. 2020

Publ. Astron. Soc. Aust.

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We present the results of a new selection technique to identify powerful ( $L_{\rm 500\,MHz} \gt 10^{27}\,\text{WHz}^{-1}$ ) radio galaxies towards the end of the Epoch of Reionisation. Our method is based on the selection of bright radio sources showing radio spectral curvature at the lowest frequency ( ${\sim}100\,\text{MHz}$ ) combined with the traditional faintness in K-band for high-redshift galaxies. This technique is only possible, thanks to the Galactic and Extra-galactic All-sky Murchison Wide-field Array survey which provides us with 20 flux measurements across the 70– $230\,\text{MHz}$ range. For this pilot project, we focus on the GAMA 09 field to demonstrate our technique. We present the results of our follow-up campaign with the Very Large Telescope, Australian Telescope Compact Array, and the Atacama Large Millimetre Array to locate the host galaxy and to determine its redshift. Of our four candidate high-redshift sources, we find two powerful radio galaxies in the $1<z<3$ range, confirm one at $z=5.55$ , and present a very tentative $z=10.15$ candidate. Their near-infrared and radio properties show that we are preferentially selecting some of the most radio luminous objects, hosted by massive galaxies very similar to powerful radio galaxies at $1<z<5$ . Our new selection and follow-up technique for finding powerful radio galaxies at $z>5.5$ has a high 25–50% success rate.

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Section: The Complex Case Of Gleam 0917mentioning

confidence: 84%

The GLEAMing of the first supermassive black holes

Drouart

Seymour

Galvin

et al. 2020

Publ. Astron. Soc. Aust.

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“…The eight GEMS listed in Table 1 were included, with continuum-subtracted spectra either from the WILMA or FTS backends. We performed the stacking following the method described in Spilker et al (2014) and Wilson et al (2017). Spectra were shifted to a common redshift of z = 3.0 according to the best source redshift from CO (C18) because the dense-gas line redshifts are poorly constrained in most cases.…”

Section: Appendix A: Stacking Analysis Of Emir Spectramentioning

confidence: 99%

Planck’s Dusty GEMS

Cañameras

Nesvadba²,

Kneißl³

et al. 2021

A&A

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We present ALMA, NOEMA, and IRAM-30 m/EMIR observations of the high-density tracer molecules HCN, HCO + , and HNC in three of the brightest lensed dusty star-forming galaxies at z 3-3.5, part of the Planck's Dusty Gravitationally Enhanced sub-Millimetre Sources (GEMS), with the aim of probing the gas reservoirs closely associated with their exceptional levels of star formation. We obtained robust detections of ten emission lines between J up = 4 and 6, as well as several additional upper flux limits. In PLCK_G244.8+54.9, the brightest source at z = 3.0, the HNC(5-4) line emission at 0.1 resolution, together with other spatially-integrated line profiles, suggests comparable distributions of dense and more diffuse gas reservoirs, at least over the most strongly magnified regions. This rules out any major effect from differential lensing. This line is blended with CN(4-3) and in this source, we measure a HNC(5-4)/CN(4-3) flux ratio of 1.76 ±0. 86. Dense-gas line profiles generally match those of mid-J CO lines, except in PLCK_G145.2+50.8, which also has dense-gas line fluxes that are relatively lower, perhaps due to fewer dense cores and more segregated dense and diffuse gas phases in this source. The HCO + /HCN 1 and HNC/HCN ∼ 1 line ratios in our sample are similar to those of nearby ultraluminous infrared galaxies (ULIRGs) and consistent with photon-dominated regions without any indication of important mechanical heating or active galactic nuclei feedback. We characterize the dense-gas excitation in PLCK_G244.8+54.9 using radiative transfer models assuming pure collisional excitation and find that mid-J HCN, HCO + , and HNC lines arise from a high-density phase with an H 2 density of n ∼ 10 5-10 6 cm −3 , although important degeneracies hinder a determination of the exact conditions. The three GEMS are consistent with extrapolations of dense-gas star-formation laws derived in the nearby Universe, adding further evidence that the extreme star-formation rates observed in the most active galaxies at z ∼ 3 are a consequence of their important dense-gas contents. The dense-gas-mass fractions traced by HCN/[CI] and HCO + /[CI] line ratios are elevated, but not exceptional as compared to other lensed dusty star-forming galaxies at z > 2, and they fall near the upper envelope of local ULIRGs. Despite the higher overall gas fractions and local gas-mass surface densities observed at high redshift, the dense-gas budget of rapidly star-forming galaxies seems to have evolved little between z ∼ 3 and z ∼ 0. Our results favor constant dense-gas depletion times in these populations, which is in agreement with theoretical models of star formation.

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“…As a result there has been little observational work surveying this line in extra-galactic sources, and most have been restricted to a few nearby starbursts, local (U)LIRGs and high-z SMG and QSO (Israel et al 2006;Weiß et al 2005;Walter et al 2011;Zhang et al 2014;Krips et al 2016). Herschel expanded the observations of the [Ci] lines in nearby galaxies with the FTS spectrometer (Kamenetzky et al 2014;Lu et al 2017;Jiao et al 2017Jiao et al , 2019Wilson et al 2017;Crocker et al 2019) but its limited sensitivity meant that the targets were mostly still (U)LIRGs or only the central regions of very nearby galaxies. The recent development of the Atacama Large Millimetre Array (ALMA) and upgrades to NOEMA have allowed an expansion of studies focused on using [Ci] as a tracer of molecular gas at high redshifts (Alaghband-Zadeh et al 2013;Bothwell et al 2017;Valentino et al 2018Valentino et al , 2020Bourne et al 2019), but what is lacking is a well defined sample of non-extreme star forming galaxies with global observations of all three main gas tracers:-12 CO(1 − 0) , [Ci] (1-0) and sub-mm observations of cold dust.…”

Section: For a Good Review)mentioning

confidence: 99%

Dust continuum, CO, and [C i] 1 − 0 lines: self-consistent H2 mass estimates and the possibility of globally CO-‘dark’ galaxies at z = 0.35

Dunne

Maddox

Vlahakis

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present ALMA observations of a small but statistically complete sample of twelve 250μm selected galaxies at z = 0.35 designed to measure their dust submillimeter continuum emission as well as their $\rm {^{12}CO(1-0)}$ and atomic carbon [Ci](3P1-3P0) spectral lines. This is the first sample of galaxies with global measures of all three H2-mass tracers and which show star formation rates (4–26 $\rm M_{\odot }$ yr−1) and infra-red luminosities ($1-6\times 10^{11}\, {\,\rm L_{\odot }\,}$) typical of star forming galaxies in their era. We find a surprising diversity of morphology and kinematic structure; one-third of the sample have evidence for interaction with nearby smaller galaxies, several sources have disjoint dust and gas morphology. Moreover two galaxies have very high $L^{\prime }_{\rm CI}$ / $L^{\prime }_{\rm {CO}}$ ratios for their global molecular gas reservoirs; if confirmed, such extreme intensity ratios in a sample of dust selected, massive star forming galaxies presents a challenge to our understanding of ISM. Finally, we use the emission of the three molecular gas tracers, to determine the carbon abundance, $\rm {X_{CI}}$ , and CO–$\rm {H_2}$ conversion αCO in our sample, using a weak prior that the gas-to-dust ratio is similar to that of the Milky Way for these massive and metal rich galaxies. Using a likelihood method which simultaneously uses all three gas tracer measurements, we find mean values and errors on the mean of $\langle {\,\alpha _{\rm {CO}}\,}\rangle =3.0\pm 0.5\, \rm {{\,\rm M_{\odot }\,}\, (K\, kms^{-1}\, pc^2)^{-1}}$ and $\langle {\,\rm {X_{CI}}\,}\rangle =1.6\pm 0.1\times 10^{-5}$ (or ${\,\alpha _{\rm {CI}}\,}=18.8\, {\,\rm {M_{\odot }\, (K\, kms^{-1}\, pc^2)^{-1}}\,}$) and ${\,\delta _{\rm {GDR}}\,}=128\pm 16$ (or ${\,\alpha _{\rm {850}}\,}=5.9\times 10^{12}\, \rm {W\, Hz^{-1}\, {\,\rm M_{\odot }\,}^{-1}}$), where our starting assumption is that these metal rich galaxies have an average gas-to-dust ratio similar to that of the Milky Way centered on ${\,\delta _{\rm {GDR}}\,}=135$.

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Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer^∗

Cited by 17 publications

References 226 publications

The GLEAMing of the first supermassive black holes

The GLEAMing of the first supermassive black holes

Planck’s Dusty GEMS

Dust continuum, CO, and [C i] 1 − 0 lines: self-consistent H2 mass estimates and the possibility of globally CO-‘dark’ galaxies at z = 0.35

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About

Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer∗

Cited by 17 publications

References 226 publications

The GLEAMing of the first supermassive black holes

The GLEAMing of the first supermassive black holes

Planck’s Dusty GEMS

Dust continuum, CO, and [C i] 1 − 0 lines: self-consistent H2 mass estimates and the possibility of globally CO-‘dark’ galaxies at z = 0.35

Contact Info

Product

Resources

About

Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer^∗