ENHANCED STAR FORMATION OF LESS MASSIVE GALAXIES IN A PROTOCLUSTER AT z = 2.5

Hayashi, Masao; Kodama, Tadayuki; Tanaka, Ichi; Shimakawa, Rhythm; Koyama, Yusei; Tadaki, Ken-ichi; Suzuki, Tomoko L.; Yamamoto, Moegi

doi:10.3847/2041-8205/826/2/l28

Cited by 37 publications

(70 citation statements)

References 36 publications

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“…We tentatively found a signature of enhanced star formation at a given stellar mass that is similarly observed in other protocluster members (Hayashi et al 2016;I. Tanaka et al 2017, in preparation).…”

Section: Moircs/subaru Nir Data: Mstar and Sfrsupporting

confidence: 77%

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA

Lee

Tanaka

Kawabe

et al. 2017

ApJ

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A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA Lee, Minju M.; Tanaka, Ichi; Kawabe, Ryohei; Kohno, Kotaro; Kodama, Tadayuki; Kajisawa, Masaru; Yun, Min S.; Nakanishi, Kouichiro; Iono, Daisuke; Tamura, Yoichi IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document VersionPublisher's PDF, also known as Version of record Publication date: 2017Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Lee, M. M., Tanaka, I., Kawabe, R., Kohno, K., Kodama, T., Kajisawa, M., ... Ivison, R. J. (2017). A Radioto-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA. The Astrophysical Journal, 842(1), [55]. DOI: 10.3847/1538-4357/aa74c2 Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons).Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim.Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. AbstractWe investigate gas contents of star-forming galaxies associated with protocluster 4C23.56 at z=2.49by using the redshifted CO(3-2) and 1.1 mm dust continuum with the Atacama Large Millimeter/submillimeter Array. The observations unveil seven CO detections out of 22 targeted Hα emitters (HAEs)and four out of 19 in 1.1 mm dust continuum. They have high stellar mass (  >Ḿ 4 10 10 M e ) and exhibit aspecific star-formation rate typical of main-sequence star-forminggalaxies atz 2.5. Different gas-mass estimators from CO(3-2) and 1.1 mm yield consistent values for simultaneous detections. The gas mass (M gas ) and gas fraction ( f gas ) are comparable to those of field galaxies, with ))  M , where a CO is the CO-to-H 2 conversion factor and A(Z) is the additional correction factor for the metallicity dependence of a CO , and á ñ =  f 0.53 0.07 gas from CO(3-2). Our measurements place a constraint on the cosmic gas density of high-z protoclusters, indicating thatthe protocluster is characterized by a gas density higher than that of the general fields by an order of magnitude. We found r~´- ( ) H M 5 10 Mpc 2 9 3 with the CO(3-2) detections. The five ALMA CO detections occur in the region ofhighest galaxy surface density,where the density positively correlates with global star-forming efficiency (SFE) and stellar mass. Such correlations possibly indicate a critical role of theenvironment on early galaxy evolution at high-z protocluste...

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Section: Moircs/subaru Nir Data: Mstar and Sfrsupporting

confidence: 77%

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA

Lee

Tanaka

Kawabe

et al. 2017

ApJ

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“…USS 1558−003 was consequently first identified with a method that is relatively more sensitive to stellar mass than star formation. Subsequent, narrowband studies by Hayashi et al (2012), Hayashi et al (2016), and Shimakawa et al (2018) with Subaru have found a total of 107 Hα-emitting galaxies (hereafter HAEs) around the radio galaxy, which supports the conclusion that this region is a cluster in formation. We present our new observations from Chandra and the LBT in §2.…”

Section: Introductionmentioning

confidence: 79%

“…There are also deep B, r ′ , and z ′ images from Subaru that were previously presented in Hayashi et al (2012). The narrowband images have a 3σ flux limit of f > 1.1 × 10 −17 erg s −1 cm −2 , which corresponds to a luminosity of L(Hα + N II) = 5.8 × 10 41 erg s −1 (Hayashi et al 2016). Shimakawa et al (2018) report that 49 of these HAEs have either spectroscopic redshifts or were also detected in redshifted Lyα narrow band images.…”

Section: Uss 1558−003 Agn Fractionmentioning

confidence: 97%

“…The large blue circles show three overdense clumps within USS 1558−003 that were identified by Hayashi et al (2012). The small purple circles are the HAEs from the Hayashi et al (2016) catalog, and the small magenta ellipses are the X-ray sources from Chandra. The red rectangles mark the five galaxies with confirmed spectroscopic redshifts from our LBT observations.…”

Section: Lbtmentioning

confidence: 99%

“…The denominator for the AGN fraction can be defined in a number of ways. We start with the catalog 100 HAEs from Hayashi et al (2016). These sources are based on an extraordinarily deep (9.7 hr) NB2315 narrowband image with the MOIRCS instrument on the Subaru telescope, J and K s broadband images, and deep F160W images obtained with the WFC3 instrument on HST.…”

Section: Uss 1558−003 Agn Fractionmentioning

confidence: 99%

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The Fraction of Active Galactic Nuclei in the USS 1558–003 Protocluster at z = 2.53

Macuga

Martini

Miller

et al. 2019

ApJ

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The incidence of Active Galactic Nuclei (AGN) with local environment is a potentially valuable probe of the mechanisms that trigger and provide fuel for accretion onto supermassive black holes. While the correlation between AGN fraction and environment has been well-studied in the local universe, AGN fractions have been measured for relatively few dense environments at high redshift. In this paper we present a measurement of the X-ray AGN fraction in the USS 1558−003 protocluster associated with the z = 2.53 radio galaxy 4C-00.62. Our measurement is based on a 100ks Chandra observation, follow-up spectroscopy from the Multi-Object Double Spectrograph on the Large Binocular Telescope, and broad and narrow band photometry. These data are sensitive to AGN more luminous than L X > 2 × 10 43 erg s −1 in the rest-frame hard X-ray band (2-10 keV). We have identified two Xray AGN at the redshift of USS 1558−003, one of which is the radio galaxy. We have determined that 2.0 +2.6 −1.3 % of the Hα emitters in the protocluster are X-ray AGN. Unlike most other high-redshift cluster progenitors studied with similar techniques, USS 1558−003 does not have a significantly higher fraction of AGN than field galaxies at similar redshifts. This lower AGN fraction is inconsistent with the expectation that the higher gas fractions at high redshift, combined with the high galaxy densities and modest relative velocities in protoclusters, should produce higher AGN fractions.

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Spectroscopic observations of PHz G237.01+42.50: A galaxy protocluster at z = 2.16 in the Cosmos field

Polletta

Soucail

Dole

et al. 2021

A&A

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The Planck satellite has identified more than 2000 protocluster candidates with extreme star formation rates (SFRs). Here, we present the spectroscopic identification of a Planck-selected protocluster located in the Cosmos field, PHz G237.01+42.50. PHz G237.01+42.50 contains a galaxy overdensity of 31 spectroscopically identified galaxies at z ≃ 2.16 (significant at 5.4σ) in a 10′ × 11′ region. The overdensity contains two substructures or protoclusters at ⟨z⟩ ≃ 2.16 and 2.195 with estimated halo masses at z = 0 of ∼5–6 × 1014 M⊙, roughly consistent with Virgo-type clusters. The overdensity total SFR, ∼4000 M⊙ yr−1, is higher than predicted by simulations but much smaller than the SFR derived from the Planck data (i.e., 10 173 M⊙ yr−1). The analysis of the Herschel data in the field, in combination with the available ancillary data, shows that such a difference is due to an effect of source alignment along the line of sight that produces a 5σ overdensity of red Herschel sources in the field. We analyze the members’ ultraviolet (UV) spectra and UV-far-infrared spectral energy distributions to derive their SFR, stellar mass, and metallicity. Galaxy members include blue star-forming galaxies and Active galactic nuclei (AGN) with SFRs and stellar masses consistent with the main sequence. Active galactic nuclei, identified through optical spectroscopy or X-ray data, represent a significant fraction (20 ± 10%) of all members of the protocluster at z = 2.16, and they are powerful enough to produce radiative feedback. The core of this protocluster, besides being denser, includes members that are, on average, more massive and star-forming and contains a larger fraction of AGN and Herschel-detected galaxies than the full sample, suggesting an environmental effect on galaxy growth. A comparison between PHz G237.01+42.50 and other protoclusters in the literature at similar redshifts reveals some common traits and differences that reflect both observational biases and a diversity in intrinsic properties that is not yet fully understood.

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ENHANCED STAR FORMATION OF LESS MASSIVE GALAXIES IN A PROTOCLUSTER AT z = 2.5

Cited by 37 publications

References 36 publications

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA

The Fraction of Active Galactic Nuclei in the USS 1558–003 Protocluster at z = 2.53

Spectroscopic observations of PHz G237.01+42.50: A galaxy protocluster at z = 2.16 in the Cosmos field

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