Giant galaxy growing from recycled gas: ALMA maps the circumgalactic molecular medium of the Spiderweb in [<scp>C i</scp>]

Emonts, Bjorn; Lehnert, M. D.; Dannerbauer, H.; Breuck, C. De; Villar-Martín, M.; Miley, G. K.; Allison, J. R.; Gullberg, B.; Hatch, N. A.; Guillard, P.; Mao, Minnie; Norris, R. P.

doi:10.1093/mnrasl/sly034

Cited by 65 publications

(86 citation statements)

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“…There are many ways to explain the nature of the extended emission seen here, including tidal tails resulting from gravitational interactions amongst galaxies, in particular through major mergers (e.g., Toomre & Toomre 1972;Barnes 1988), or an expanding shell of ionized gas (as seen for example in local gas-rich galaxies, e.g., Heiles 1979;McClure-Griffiths et al 2002). Extended gas emission has been detected in some proto-clusters through the CO(1-0) transition (Emonts et al 2016;Dannerbauer et al 2017), the CO(3-4) transition (Ginolfi et al 2017), and in [Ci] (Emonts et al 2018), and it has also been statistically detected surrounding z = 4-7 galaxies through stacking analyses (Fujimoto et al 2019;Ginolfi et al 2020). The extended gas in these systems could affect the evolution of the embed-ded galaxies (see e.g.…”

Section: Extended [Cii] Emissionmentioning

confidence: 99%

Megaparsec-scale structure around the protocluster core SPT2349–56 at z = 4.3

Hill

Chapman

Scott

et al. 2020

Monthly Notices of the Royal Astronomical Society

139

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We present an extensive ALMA spectroscopic follow-up programme of the $z\, {=}\, 4.3$ structure SPT2349–56, one of the most actively star-forming protocluster cores known, to identify additional members using their [C ii] 158 μm and CO(4–3) lines. In addition to robustly detecting the 14 previously published galaxies in this structure, we identify a further 15 associated galaxies at $z\, {=}\, 4.3$, resolving 55$\, {\pm }\,$5 per cent of the 870 μm flux density at 0.5 arcsec resolution compared to 21 arcsec single-dish data. These galaxies are distributed into a central core containing 23 galaxies extending out to 300 kpc in diameter, and a northern extension, offset from the core by 400 kpc, containing three galaxies. We discovered three additional galaxies in a red Herschel-SPIRE source 1.5 Mpc from the main structure, suggesting the existence of many other sources at the same redshift as SPT2349–56 that are not yet detected in the limited coverage of our data. An analysis of the velocity distribution of the central galaxies indicates that this region may be virialized with a mass of (9$\pm 5)\, {\times }\, 10^{12}$ M⊙, while the two offset galaxy groups are about 30 and 60 per cent less massive and show significant velocity offsets from the central group. We calculate the [C ii] and far-infrared number counts, and find evidence for a break in the [C ii] luminosity function. We estimate the average SFR density within the region of SPT2349–56 containing single-dish emission (a proper diameter of 720 kpc), assuming spherical symmetry, to be roughly 4$\, {\times }\, 10^4$ M⊙ yr−1 Mpc−3; this may be an order of magnitude greater than the most extreme examples seen in simulations.

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Section: Extended [Cii] Emissionmentioning

confidence: 99%

Megaparsec-scale structure around the protocluster core SPT2349–56 at z = 4.3

Hill

Chapman

Scott

et al. 2020

Monthly Notices of the Royal Astronomical Society

139

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“…Here, Q 10 is the excitation factor and depends on the temperature and density of the gas, as well as on the intensity of the radiation field impinging upon it ). Without having any other molecular lines (e.g., CO or [C i](2-1)), we cannot constrain this parameter and we assumed the median value of Q 10 = 0.48 (Papadopoulos & Greve 2004;Emonts et al 2018). Finally, A 10 is the Einstein A-coefficient, A 10 = 7.93 × 10 −8 s −1 .…”

Section: A Normal Star-forming Galaxy?mentioning

confidence: 99%

ALMA and MUSE observations reveal a quiescent multi-phase circumgalactic medium around the z ≃ 3.6 radio galaxy 4C 19.71

Falkendal

Lehnert

Vernet

et al. 2021

A&A

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We present MUSE at VLT imaging spectroscopy of rest-frame ultraviolet emission lines and ALMA observations of the [C I] 3P1−3P0 emission line, probing both the ionized and diffuse molecular medium around the radio galaxy 4C 19.71 at z ≃ 3.6. This radio galaxy has extended Lyα emission over a region ∼100 kpc in size preferentially oriented along the axis of the radio jet. Faint Lyα emission extends beyond the radio hot spots. We also find extended C IV and He II emission over a region of ∼150 kpc in size, where the most distant emission lies ∼40 kpc beyond the north radio lobe and has narrow full width half maximum (FWHM) line widths of ∼180 km s−1 and a small relative velocity offset Δv ∼ 130 km s−1 from the systemic redshift of the radio galaxy. The [C I] is detected in the same region with FWHM ∼ 100 km s−1 and Δv ∼ 5 km s−1, while [C I] is not detected in the regions south of the radio galaxy. We interpret the coincidence in the northern line emission as evidence of relatively quiescent multi-phase gas residing within the halo at a projected distance of ∼75 kpc from the host galaxy. To test this hypothesis, we performed photoionization and photo-dissociated region (PDR) modeling, using the code Cloudy, of the three emission line regions: the radio galaxy proper and the northern and southern regions. We find that the [C I]/C IVλλ1548,1551 and C IVλλ1548,1551/He II ratios of the two halo regions are consistent with a PDR or ionization front in the circumgalactic medium likely energized by photons from the active galactic nuclei. This modeling is consistent with a relatively low metallicity, 0.03 < [Z/Z⊙] < 0.1, and diffuse ionization with an ionization parameter (proportional to the ratio of the photon number density and gas density) of log U ∼ −3 for the two circumgalactic line emission regions. Using rough mass estimates for the molecular and ionized gas, we find that the former may be tracing ≈2−4 orders of magnitude more mass. As our data are limited in signal-to-noise due to the faintness of the line, deeper [C I] observations are required to trace the full extent of this important component in the circumgalactic medium.

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“…The Spiderweb protocluster is a well-surveyed region, with numerous studies in addition to those already mentioned, e.g., MIPS 24 µm imaging with the Spitzer Space Telescope (Mayo et al 2012;Koyama et al 2013a,b), LABOCA 870 µm imaging with the APEX telescope (Dannerbauer et al 2014), CO(1 − 0) observation with ATCA (Emonts et al 2016;Dannerbauer et al 2017;Emonts et al 2018), and CO(3 − 2) observation with ALMA (Tadaki et al in preparation).…”

Section: Other Resourcesmentioning

confidence: 99%

MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

Shimakawa

Koyama

Röttgering

et al. 2018

Monthly Notices of the Royal Astronomical Society

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This paper is the second in a series presenting the results of our deep Hα-line survey towards protoclusters at z > 2, based on narrow-band imaging with the Subaru Telescope. This work investigates massive galaxies in a protocluster region associated with a radio galaxy (PKS 1138−262), the Spiderweb galaxy, at z = 2.2. Our 0.5 mag deeper narrow-band imaging than previous surveys collects a total of 68 Hα emitters (HAE). 17 out of the 68 are newly discovered protocluster members. First, a very high characteristic stellar mass of M * = 10 11.73 M is measured from a Schechter function fit to the mass distribution of HAEs. Together with the Chandra X-ray data, we find that four out of six massive HAEs (M > 10 11 M ) show bright X-ray emission, suggesting that they host active galactic nuclei (AGNs). Their mass estimates, therefore, would be affected by the nuclear emission from AGNs. Notably, the X-ray detected HAEs are likely positioned near the boundary between star-forming and quiescent populations in the rest-frame UV J plane. Moreover, our deep narrow-band data succeed in probing the bright Hα (+[Nii]) line nebula of the Spiderweb galaxy extending over ∼ 100 physical kpc. These results suggest that the massive galaxies in the Spiderweb protocluster are on the way to becoming the bright red sequence objects seen in local galaxy clusters, where AGNs might play an essential role in their quenching processes. Though a more statistical database is needed to build a general picture.

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Giant galaxy growing from recycled gas: ALMA maps the circumgalactic molecular medium of the Spiderweb in [C i]

Cited by 65 publications

References 50 publications

Megaparsec-scale structure around the protocluster core SPT2349–56 at z = 4.3

Megaparsec-scale structure around the protocluster core SPT2349–56 at z = 4.3

ALMA and MUSE observations reveal a quiescent multi-phase circumgalactic medium around the z ≃ 3.6 radio galaxy 4C 19.71

MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

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