Discovery of a rich cluster at z = 1.63 using the rest-frame 1.6 μm "stellar bump sequence" method

Adam Muzzin, Gillian Wilson, Ricardo Demarco, Chris Lidman, Julie Nantais, Henk Hoekstra, H. K C Yee, Alessandro Rettura

Resultado de la investigación: Article

62 Citas (Scopus)

Resumen

We present a new two-color algorithm, the "Stellar Bump Sequence" (SBS), that is optimized for robustly identifying candidate high-redshift galaxy clusters in combined wide-field optical and mid-infrared (MIR) data. The SBS algorithm is a fusion of the well-tested cluster red-sequence method of Gladders & Yee with the MIR 3.6 μm-4.5 μm cluster detection method developed by Papovich. As with the cluster red-sequence method, the SBS identifies candidate overdensities within 3.6 μm-4.5 μm color slices, which are the equivalent of a rest-frame 1.6 μm stellar bump "red-sequence." In addition to employing the MIR colors of galaxies, the SBS algorithm incorporates an optical/MIR (z′-3.6 μm) color cut. This cut effectively eliminates foreground 0.2 <z < 0.4 galaxies which have 3.6 μm-4.5 μm colors that are similarly red as z > 1.0 galaxies and add noise when searching for high-redshift galaxy overdensities. We demonstrate using the z ∼ 1 GCLASS cluster sample that similar to the red sequence, the stellar bump sequence appears to be a ubiquitous feature of high-redshift clusters, and that within that sample the color of the stellar bump sequence increases monotonically with redshift and provides photometric redshifts accurate to Δz = 0.05. We apply the SBS method in the XMM-LSS SWIRE field and show that it robustly recovers the majority of confirmed optical, MIR, and X-ray-selected clusters at z > 1.0 in that field. Lastly, we present confirmation of SpARCS J022427-032354 at z = 1.63, a new cluster detected with the method and confirmed with 12 high-confidence spectroscopic redshifts obtained using FORS2 on the Very Large Telescope. We conclude with a discussion of future prospects for using the algorithm.

Idioma originalEnglish
Número de artículo39
PublicaciónAstrophysical Journal
Volumen767
N.º1
DOI
EstadoPublished - 10 abr 2013

Huella dactilar

color
galaxies
future prospect
detection method
large-scale structure of the universe
method
XMM-Newton telescope
confidence
fusion
telescopes
x rays

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Muzzin, Adam ; Wilson, Gillian ; Demarco, Ricardo ; Lidman, Chris ; Nantais, Julie ; Hoekstra, Henk ; Yee, H. K C ; Rettura, Alessandro. / Discovery of a rich cluster at z = 1.63 using the rest-frame 1.6 μm "stellar bump sequence" method. En: Astrophysical Journal. 2013 ; Vol. 767, N.º 1.
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abstract = "We present a new two-color algorithm, the {"}Stellar Bump Sequence{"} (SBS), that is optimized for robustly identifying candidate high-redshift galaxy clusters in combined wide-field optical and mid-infrared (MIR) data. The SBS algorithm is a fusion of the well-tested cluster red-sequence method of Gladders & Yee with the MIR 3.6 μm-4.5 μm cluster detection method developed by Papovich. As with the cluster red-sequence method, the SBS identifies candidate overdensities within 3.6 μm-4.5 μm color slices, which are the equivalent of a rest-frame 1.6 μm stellar bump {"}red-sequence.{"} In addition to employing the MIR colors of galaxies, the SBS algorithm incorporates an optical/MIR (z′-3.6 μm) color cut. This cut effectively eliminates foreground 0.2 1.0 galaxies and add noise when searching for high-redshift galaxy overdensities. We demonstrate using the z ∼ 1 GCLASS cluster sample that similar to the red sequence, the stellar bump sequence appears to be a ubiquitous feature of high-redshift clusters, and that within that sample the color of the stellar bump sequence increases monotonically with redshift and provides photometric redshifts accurate to Δz = 0.05. We apply the SBS method in the XMM-LSS SWIRE field and show that it robustly recovers the majority of confirmed optical, MIR, and X-ray-selected clusters at z > 1.0 in that field. Lastly, we present confirmation of SpARCS J022427-032354 at z = 1.63, a new cluster detected with the method and confirmed with 12 high-confidence spectroscopic redshifts obtained using FORS2 on the Very Large Telescope. We conclude with a discussion of future prospects for using the algorithm.",
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Discovery of a rich cluster at z = 1.63 using the rest-frame 1.6 μm "stellar bump sequence" method. / Muzzin, Adam; Wilson, Gillian; Demarco, Ricardo; Lidman, Chris; Nantais, Julie; Hoekstra, Henk; Yee, H. K C; Rettura, Alessandro.

En: Astrophysical Journal, Vol. 767, N.º 1, 39, 10.04.2013.

Resultado de la investigación: Article

TY - JOUR

T1 - Discovery of a rich cluster at z = 1.63 using the rest-frame 1.6 μm "stellar bump sequence" method

AU - Muzzin, Adam

AU - Wilson, Gillian

AU - Demarco, Ricardo

AU - Lidman, Chris

AU - Nantais, Julie

AU - Hoekstra, Henk

AU - Yee, H. K C

AU - Rettura, Alessandro

PY - 2013/4/10

Y1 - 2013/4/10

N2 - We present a new two-color algorithm, the "Stellar Bump Sequence" (SBS), that is optimized for robustly identifying candidate high-redshift galaxy clusters in combined wide-field optical and mid-infrared (MIR) data. The SBS algorithm is a fusion of the well-tested cluster red-sequence method of Gladders & Yee with the MIR 3.6 μm-4.5 μm cluster detection method developed by Papovich. As with the cluster red-sequence method, the SBS identifies candidate overdensities within 3.6 μm-4.5 μm color slices, which are the equivalent of a rest-frame 1.6 μm stellar bump "red-sequence." In addition to employing the MIR colors of galaxies, the SBS algorithm incorporates an optical/MIR (z′-3.6 μm) color cut. This cut effectively eliminates foreground 0.2 1.0 galaxies and add noise when searching for high-redshift galaxy overdensities. We demonstrate using the z ∼ 1 GCLASS cluster sample that similar to the red sequence, the stellar bump sequence appears to be a ubiquitous feature of high-redshift clusters, and that within that sample the color of the stellar bump sequence increases monotonically with redshift and provides photometric redshifts accurate to Δz = 0.05. We apply the SBS method in the XMM-LSS SWIRE field and show that it robustly recovers the majority of confirmed optical, MIR, and X-ray-selected clusters at z > 1.0 in that field. Lastly, we present confirmation of SpARCS J022427-032354 at z = 1.63, a new cluster detected with the method and confirmed with 12 high-confidence spectroscopic redshifts obtained using FORS2 on the Very Large Telescope. We conclude with a discussion of future prospects for using the algorithm.

AB - We present a new two-color algorithm, the "Stellar Bump Sequence" (SBS), that is optimized for robustly identifying candidate high-redshift galaxy clusters in combined wide-field optical and mid-infrared (MIR) data. The SBS algorithm is a fusion of the well-tested cluster red-sequence method of Gladders & Yee with the MIR 3.6 μm-4.5 μm cluster detection method developed by Papovich. As with the cluster red-sequence method, the SBS identifies candidate overdensities within 3.6 μm-4.5 μm color slices, which are the equivalent of a rest-frame 1.6 μm stellar bump "red-sequence." In addition to employing the MIR colors of galaxies, the SBS algorithm incorporates an optical/MIR (z′-3.6 μm) color cut. This cut effectively eliminates foreground 0.2 1.0 galaxies and add noise when searching for high-redshift galaxy overdensities. We demonstrate using the z ∼ 1 GCLASS cluster sample that similar to the red sequence, the stellar bump sequence appears to be a ubiquitous feature of high-redshift clusters, and that within that sample the color of the stellar bump sequence increases monotonically with redshift and provides photometric redshifts accurate to Δz = 0.05. We apply the SBS method in the XMM-LSS SWIRE field and show that it robustly recovers the majority of confirmed optical, MIR, and X-ray-selected clusters at z > 1.0 in that field. Lastly, we present confirmation of SpARCS J022427-032354 at z = 1.63, a new cluster detected with the method and confirmed with 12 high-confidence spectroscopic redshifts obtained using FORS2 on the Very Large Telescope. We conclude with a discussion of future prospects for using the algorithm.

KW - galaxies: clusters: general

KW - galaxies: high-redshift

KW - infrared: galaxies

KW - large-scale structure of universe

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