Discovery of molecular gas fueling galaxy growth in a protocluster at <i>z</i> = 1.7

D’Amato, Q.; Gilli, R.; Prandoni, I.; Vignali, C.; Massardi, M.; Mignoli, M.; Cucciati, O.; Morishita, Takahiro; Decarli, Roberto; Brusa, M.; Calura, F.; Balmaverde, B.; Chiaberge, M.; Liuzzo, E.; Nanni, Riccardo; Peca, Alessandro; Pensabene, Antonio; Tozzi, P.; Norman, C.

doi:10.1051/0004-6361/202038711

Cited by 23 publications

(16 citation statements)

References 29 publications

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“…[46]) of its major stellar mass building. Indeed, we note that the derived SFR implies that the molecular gas reservoir measured by [16] will be depleted in ∼3.5 × 10 8 yr. Moreover, assuming that the BH is accreting with an efficiency η = 0.3 (as assumed by [15] and as generally thought for BHs powering jetted AGN; refs.…”

Section: Sed Fitting: a Proto-bcg Caught At The Peak Of Its Stellar Mass Buildingmentioning

confidence: 78%

“…Based on Atacama Large Millimeter Array (ALMA) observations of the CO(2-1) transition line, ref. [16] reported the discovery of three new gas-rich members (magenta circles in Figure 1), in addition to a large molecular gas reservoir (M H 2 ∼ 2 × 10 11 M ) distributed in a ∼20-30 kpc structure around the FRII host galaxy and rotating perpendicularly to the radio jets (at least in projection). Furthermore, ref.…”

Section: The J1030 Protocluster: Summary Of Previous Resultsmentioning

confidence: 99%

“…Furthermore, ref. [16] demonstrated that the overdensity will collapse in a cluster of at least 10 14 M at z = 0, and that the FRII galaxy will likely evolve into the future brightest cluster galaxy (BCG). Ref.…”

Section: The J1030 Protocluster: Summary Of Previous Resultsmentioning

confidence: 99%

“…It is also covered by the Spitzer Infrared array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) mosaics [24], and Hershel Photodetecting Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) observations [25]. The innermost region is covered by deep Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) and Wide Field Camera 3 (WFC3) observations ( [16,26]). In this work we exploit available photometry to perform a spectral energy distribution (SED) analysis of the FRII host galaxy (Section 3.1).…”

Section: Observations and Data Reduction 21 Broadband Optical/ir Photometrymentioning

confidence: 99%

“…We derived 3.3-mm photometry from proprietary ALMA observations, composed by a mosaic of three pointings performed in Band 3 (84-116 GHz) during Cycle 6 (project ID: 2018.1.01601.S, PI: R. Gilli). Details about the scheduling blocks and calibrators can be found in [16]. The 2 × 4 GHz spectral windows have been set to cover the frequency ranges 84.1-87.7 GHz and 96.1-99.9 GHz, respectively.…”

Section: Alma Photometrymentioning

confidence: 99%

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Multi-Wavelength Study of a Proto-BCG at z = 1.7

et al. 2021

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In this work we performed a spectral energy distribution (SED) analysis in the optical/infrared band of the host galaxy of a proto-brightest bluster galaxy (BCG, NVSS J103023 + 052426) in a proto-cluster at z = 1.7. We found that it features a vigorous star formation rate (SFR) of ∼570 M⊙/yr and a stellar mass of M*∼3.7×1011M⊙; the high corresponding specific SFR = 1.5±0.5Gyr−1 classifies this object as a starburst galaxy that will deplete its molecular gas reservoir in ∼3.5×108 yr. Thus, this system represents a rare example of a proto-BCG caught during the short phase of its major stellar mass assembly. Moreover, we investigated the nature of the host galaxy emission at 3.3 mm. We found that it originates from the cold dust in the interstellar medium, even though a minor non-thermal AGN contribution cannot be completely ruled out. Finally, we studied the polarized emission of the lobes at 1.4 GHz. We unveiled a patchy structure where the polarization fraction increases in the regions in which the total intensity shows a bending morphology; in addition, the magnetic field orientation follows the direction of the bendings. We interpret these features as possible indications of an interaction with the intracluster medium. This strengthens the hypothesis of positive AGN feedback, as inferred in previous studies of this object on the basis of X-ray/mm/radio analysis. In this scenario, the proto-BCG heats the surrounding medium and possibly enhances the SFR in nearby galaxies.

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Section: Sed Fitting: a Proto-bcg Caught At The Peak Of Its Stellar Mass Buildingmentioning

confidence: 78%

Section: The J1030 Protocluster: Summary Of Previous Resultsmentioning

confidence: 99%

Section: The J1030 Protocluster: Summary Of Previous Resultsmentioning

confidence: 99%

Section: Observations and Data Reduction 21 Broadband Optical/ir Photometrymentioning

confidence: 99%

Section: Alma Photometrymentioning

confidence: 99%

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Multi-Wavelength Study of a Proto-BCG at z = 1.7

et al. 2021

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Hosts and environments: a (large-scale) radio history of AGN and star-forming galaxies

Magliocchetti

2022

Astron Astrophys Rev

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Despite their relative sparseness, during the recent years it has become more and more clear that extragalactic radio sources (both AGN and star-forming galaxies) constitute an extremely interesting mix of populations, not only because of their intrinsic value, but also for their fundamental role in shaping our universe the way we see it today. Indeed, radio-active AGN are now thought to be the main players involved in the evolution of massive galaxies and clusters. At the same time, thanks to the possibility of being observed up to very high redshifts, radio galaxies can also provide crucial information on both the star-formation history of our universe and on its large-scale structure properties and their evolution. In the light of present and forthcoming facilities such as LOFAR, MeerKAT and SKA that will probe the radio sky to unprecedented depths and widths, this review aims at providing the current state of the art on our knowledge of extragalactic radio sources in connection with their hosts, large-scale environments and cosmological context.

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Planck 2018 results

Aghanim

Akrami

Ashdown

et al. 2020

A&A

217

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This paper presents the High Frequency Instrument (HFI) data processing procedures for the Planck 2018 release. Major improvements in mapmaking have been achieved since the previous Planck 2015 release, many of which were used and described already in an intermediate paper dedicated to the Planck polarized data at low multipoles. These improvements enabled the first significant measurement of the reionization optical depth parameter using Planck-HFI data. This paper presents an extensive analysis of systematic effects, including the use of end-to-end simulations to facilitate their removal and characterize the residuals. The polarized data, which presented a number of known problems in the 2015 Planck release, are very significantly improved, especially the leakage from intensity to polarization. Calibration, based on the cosmic microwave background (CMB) dipole, is now extremely accurate and in the frequency range 100–353 GHz reduces intensity-to-polarization leakage caused by calibration mismatch. The Solar dipole direction has been determined in the three lowest HFI frequency channels to within one arc minute, and its amplitude has an absolute uncertainty smaller than 0.35 μK, an accuracy of order 10−4. This is a major legacy from the Planck HFI for future CMB experiments. The removal of bandpass leakage has been improved for the main high-frequency foregrounds by extracting the bandpass-mismatch coefficients for each detector as part of the mapmaking process; these values in turn improve the intensity maps. This is a major change in the philosophy of “frequency maps”, which are now computed from single detector data, all adjusted to the same average bandpass response for the main foregrounds. End-to-end simulations have been shown to reproduce very well the relative gain calibration of detectors, as well as drifts within a frequency induced by the residuals of the main systematic effect (analogue-to-digital convertor non-linearity residuals). Using these simulations, we have been able to measure and correct the small frequency calibration bias induced by this systematic effect at the 10−4 level. There is no detectable sign of a residual calibration bias between the first and second acoustic peaks in the CMB channels, at the 10−3 level.

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Discovery of molecular gas fueling galaxy growth in a protocluster at z = 1.7

Cited by 23 publications

References 29 publications

Multi-Wavelength Study of a Proto-BCG at z = 1.7

Multi-Wavelength Study of a Proto-BCG at z = 1.7

Hosts and environments: a (large-scale) radio history of AGN and star-forming galaxies

Planck 2018 results

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