Shapes and alignments of dark matter haloes and their brightest cluster galaxies in 39 strong lensing clusters

Okabe, Takao; Oguri, Masamune; Peirani, Sébastien; Suto, Yasushi; Dubois, Yohan; Pichon, Christophe; Kitayama, Tetsu; Sasaki, Shin; Nishimichi, Takahiro

doi:10.1093/mnras/staa1479

“…tighter alignment than that reported by Durret et al (2019), who found an alignment for 12 out of 21 BCGs (57%) between redshifts 0.21 and 0.89. Okabe et al (2020) study the alignment of 45 dark matter (DM) haloes and their BCGs up to z = 0.97, and find that BCGs tend to be well aligned with their DM haloes, with a mean difference of 22.2 ± 3.9 • . A similar study was done by Ragone-Figueroa et al (2020) on the alignment of BCGs both with the distribution of cluster galaxies and DM haloes, by analyzing cosmological hydro-simulations of 24 clusters.…”

Section: Discussionmentioning

confidence: 99%

Physical properties of brightest cluster galaxies up to redshift 1.80 based on HST data

Chu

¹

,

Durret

²

,

Márquez

³

2021

A&A

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Context. Brightest cluster galaxies (BCGs) grow by accreting numerous smaller galaxies, and can be used as tracers of cluster formation and evolution in the cosmic web. However, there is still controversy regarding the main epoch of formation of BCGs; some authors believe they already formed before redshift z = 2, while others find that they are still evolving at more recent epochs. Aims. We study the physical properties of a large sample of BCGs covering a wide redshift range up to z = 1.8 and analyzed in a homogeneous way, to see if their characteristics vary with redshift. As a first step we also present a new tool to determine for each cluster which galaxy is the BCG. Methods. For a sample of 137 clusters with HST images in the optical and/or infrared, we analyzed the BCG properties by applying GALFIT with one or two Sérsic components. For each BCG we thus computed the Sérsic index, effective radius, major axis position angle, and surface brightness. We then searched for correlations of these quantities with redshift. Results. We find that the BCGs follow the Kormendy relation (between the effective radius and the mean surface brightness), with a slope that remains constant with redshift, but with a variation with redshift of the ordinate at the origin. Although the trends are faint, we find that the absolute magnitudes and the effective radii tend to become respectively brighter and bigger with decreasing redshift. On the other hand, we find no significant correlation of the mean surface brightnesses or Sérsic indices with redshift. The major axes of the cluster elongations and of the BCGs agree within 30° for 73% of our clusters at redshift z ≤ 0.9. Conclusions. Our results agree with the BCGs being mainly formed before redshift z = 2. The alignment of the major axes of BCGs with their clusters agree with the general idea that BCGs form at the same time as clusters by accreting matter along the filaments of the cosmic web.

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“…We also use the large-area low-resolution lens model produced by Merten et al (2011) in MACS0416 and MACS1149, where the identified sources are out of the coverage of the CATS products. For sources detected in the CLASH and RELICS cluster fields, we use all of the available lens models on the MAST high-level science product database, including those produced by CATS (Richard et al 2014), Zitrin-dPIEeNFW andLight-Traces-Mass (Zitrin et al 2013, 2015), and GLAFIC (Oguri 2010;Kawamata et al 2016;Okabe et al 2020).…”

Section: Lens Models and Magnificationmentioning

confidence: 99%

Extensive Lensing Survey of Optical and Near-infrared Dark Objects (El Sonido): HST H-faint Galaxies behind 101 Lensing Clusters

Sun

¹

,

Egami

²

,

Pérez‐González

³

et al. 2021

ApJ

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We present a Spitzer/IRAC survey of H-faint (H 160 ≳ 26.4, < 5σ) sources in 101 lensing cluster fields. Across a CANDELS/Wide-like survey area of ∼648 arcmin2 (effectively ∼221 arcmin2 in the source plane), we have securely discovered 53 sources in the IRAC Channel-2 band (CH2, 4.5 μm; median CH2 = 22.46 ± 0.11 AB mag) that lack robust HST/WFC3-IR F160W counterparts. The most remarkable source in our sample, namely ES-009 in the field of Abell 2813, is the brightest H-faint galaxy at 4.5 μm known so far (CH2 = 20.48 ± 0.03 AB mag). We show that the H-faint sources in our sample are massive (median M star = 1010.3±0.3 M ⊙), star-forming (median star formation rate = 100 − 40 + 60 M ⊙ yr−1), and dust-obscured (A V = 2.6 ± 0.3) galaxies around a median photometric redshift of z = 3.9 ± 0.4. The stellar continua of 14 H-faint galaxies can be resolved in the CH2 band, suggesting a median circularized effective radius (R e,circ; lensing corrected) of 1.9 ± 0.2 kpc and <1.5 kpc for the resolved and whole samples, respectively. This is consistent with the sizes of massive unobscured galaxies at z ∼ 4, indicating that H-faint galaxies represent the dusty tail of the distribution of a wider galaxy population. Comparing with the ALMA dust continuum sizes of similar galaxies reported previously, we conclude that the heavy dust obscuration in H-faint galaxies is related to the compactness of both stellar and dust continua (R e,circ ∼ 1 kpc). These H-faint galaxies make up 16 − 7 + 13 % of the galaxies in the stellar-mass range of 1010 − 1011.2 M ⊙ at z = 3 ∼ 5, contributing to 8 − 4 + 8 % of the cosmic star formation rate density in this epoch and likely tracing the early phase of massive galaxy formation.

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“…We also use the large-area low-resolution lens model produced by Merten et al (2011) in MACS0416 and MACS1149, where the identified sources are out of the coverage of the CATS products. For sources detected in the CLASH and RELICS cluster fields, we use all of the available lens models on the MAST high-level science product database, including those produced by CATS (Richard et al 2014), Zitrin-dPIEeNFW and Light-Traces-Mass (Zitrin et al 2013(Zitrin et al , 2015, and GLAFIC (Oguri 2010;Kawamata et al 2016;Okabe et al 2020).…”

Section: Lens Models and Magnificationmentioning

confidence: 99%

Extensive Lensing Survey of Optical and Near-Infrared Dark Objects (El Sonido): HST H-Faint Galaxies behind 101 Lensing Clusters

Sun,

Egami,

Pérez-González

et al. 2021

Preprint

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We present a Spitzer /IRAC survey of H-faint (H 160 26.4, < 5σ) sources in 101 lensing cluster fields. Across a CANDELS/Wide-like survey area of ∼648 arcmin 2 (effectively ∼221 arcmin 2 in the source plane), we have securely discovered 53 sources in the IRAC Channel-2 band (CH2, 4.5 µm; median CH2=22.46±0.11 AB mag) that lack robust HST /WFC3-IR F160W counterparts. The most remarkable source in our sample, namely ES-009 in the field of Abell 2813, is the brightest H-faint galaxy at 4.5 µm known so far (CH2 = 20.48 ± 0.03 AB mag). We show that the H-faint sources in our sample are massive (median M star = 10 10.3±0.3 M ), star-forming (median star formation rate = 100 +60 −40 M yr −1 ) and dust-obscured (A V = 2.6 ± 0.3) galaxies around a median photometric redshift of z = 3.9±0.4. The stellar continua of 14 H-faint galaxies can be resolved in the CH2 band, suggesting a median circularized effective radius (R e,circ ; lensing corrected) of 1.9 ± 0.2 kpc and < 1.5 kpc for the resolved and whole samples, respectively. This is consistent with the sizes of massive unobscured galaxies at z ∼ 4, indicating that H-faint galaxies represent the dusty tail of the distribution of a wider galaxy population. Comparing with the ALMA dust continuum sizes of similar galaxies reported previously, we conclude that the heavy dust obscuration in H-faint galaxies is related to the compactness of both stellar and dust continua (R e,circ ∼ 1 kpc). These H-faint galaxies make up 16 +13−7 % of the galaxies in the stellar mass range of 10 10 − 10 11.2 M at z = 3 ∼ 5, contributing to 8 +8 −4 % of the cosmic star formation rate density in this epoch and likely tracing the early phase of massive galaxy formation.

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Shapes and alignments of dark matter haloes and their brightest cluster galaxies in 39 strong lensing clusters

Cited by 41 publications

References 83 publications

Physical properties of brightest cluster galaxies up to redshift 1.80 based on HST data

Physical properties of brightest cluster galaxies up to redshift 1.80 based on HST data

Extensive Lensing Survey of Optical and Near-infrared Dark Objects (El Sonido): HST H-faint Galaxies behind 101 Lensing Clusters

Extensive Lensing Survey of Optical and Near-Infrared Dark Objects (El Sonido): HST H-Faint Galaxies behind 101 Lensing Clusters

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