SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts

M. L. N. Ashby; S. P. Willner; G. G. Fazio; J.-S. Huang; R. Arendt; P. Barmby; G. Barro; E. F. Bell; R. Bouwens; A. Cattaneo; D. Croton; R. Davé; J. S. Dunlop; E. Egami; S. Faber; K. Finlator; N. A. Grogin; P. Guhathakurta; L. Hernquist; J. L. Hora; G. Illingworth; A. Kashlinsky; A. M. Koekemoer; D. C. Koo; I. Labbé; Y. Li; L. Lin; H. Moseley; K. Nandra; J. Newman; K. Noeske; M. Ouchi; M. Peth; D. Rigopoulou; B. Robertson; V. Sarajedini; L. Simard; H. A. Smith; Z. Wang; R. Wechsler; B. Weiner; G. Wilson; S. Wuyts; T. Yamada; H. Yan

doi:10.1088/0004-637X/769/1/80

SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts

M. L. N. Ashby, S. P. Willner, G. G. Fazio, J.-S. Huang, R. Arendt, P. Barmby, G. Barro, E. F. Bell, R. Bouwens, A. Cattaneo, D. Croton, R. Davé, J. S. Dunlop, E. Egami, S. Faber, K. Finlator, N. A. Grogin, P. Guhathakurta, L. Hernquist, J. L. HoraG. Illingworth, A. Kashlinsky, A. M. Koekemoer, D. C. Koo, I. Labbé, Y. Li, L. Lin, H. Moseley, K. Nandra, J. Newman, K. Noeske, M. Ouchi, M. Peth, D. Rigopoulou, B. Robertson, V. Sarajedini, L. Simard, H. A. Smith, Z. Wang, R. Wechsler, B. Weiner, G. Wilson, S. Wuyts, T. Yamada, H. Yan

Department of Physics

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226 Citations (SciVal)

Abstract

The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalactic
science fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the Hubble
Deep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg2 to a depth of 26 AB mag
(3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5μm. Because of its uniform depth of
coverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variance
than a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediate
to high redshifts (z = 2–7) with a built-in means of assessing the impact of cosmic variance on the individual fields.
Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six-month
intervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. This
paper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts for
the more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations.
Discrete IRAC sources contribute 5.6 ± 1.0 and 4.4 ± 0.8 nW m−2 sr−1 at 3.6 and 4.5μm to the diffuse cosmic
infrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated from
DIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come from
a diffuse component.

Original language	English
Number of pages	27
Journal	Astrophysical Journal
Volume	769
Issue number	1
Early online date	6 May 2013
DOIs	https://doi.org/10.1088/0004-637X/769/1/80
Publication status	Published - 20 May 2013

Keywords

galaxies: high redshift
infrared: galaxies
surveys

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10.1088/0004-637X/769/1/80

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Ashby, M. L. N., Willner, S. P., Fazio, G. G., Huang, J.-S., Arendt, R., Barmby, P., Barro, G., Bell, E. F., Bouwens, R., Cattaneo, A., Croton, D., Davé, R., Dunlop, J. S., Egami, E., Faber, S., Finlator, K., Grogin, N. A., Guhathakurta, P., Hernquist, L., ... Yan, H. (2013). SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts. Astrophysical Journal, 769(1). https://doi.org/10.1088/0004-637X/769/1/80

Ashby, MLN, Willner, SP, Fazio, GG, Huang, J-S, Arendt, R, Barmby, P, Barro, G, Bell, EF, Bouwens, R, Cattaneo, A, Croton, D, Davé, R, Dunlop, JS, Egami, E, Faber, S, Finlator, K, Grogin, NA, Guhathakurta, P, Hernquist, L, Hora, JL, Illingworth, G, Kashlinsky, A, Koekemoer, AM, Koo, DC, Labbé, I, Li, Y, Lin, L, Moseley, H, Nandra, K, Newman, J, Noeske, K, Ouchi, M, Peth, M, Rigopoulou, D, Robertson, B, Sarajedini, V, Simard, L, Smith, HA, Wang, Z, Wechsler, R, Weiner, B, Wilson, G, Wuyts, S, Yamada, T & Yan, H 2013, 'SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts', Astrophysical Journal, vol. 769, no. 1. https://doi.org/10.1088/0004-637X/769/1/80

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title = "SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts",

abstract = "The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalacticscience fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the HubbleDeep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg2 to a depth of 26 AB mag(3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5μm. Because of its uniform depth ofcoverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variancethan a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediateto high redshifts (z = 2–7) with a built-in means of assessing the impact of cosmic variance on the individual fields.Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six-monthintervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. Thispaper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts forthe more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations.Discrete IRAC sources contribute 5.6 ± 1.0 and 4.4 ± 0.8 nW m−2 sr−1 at 3.6 and 4.5μm to the diffuse cosmicinfrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated fromDIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come froma diffuse component.",

keywords = "galaxies: high redshift, infrared: galaxies, surveys",

author = "Ashby, {M. L. N.} and Willner, {S. P.} and Fazio, {G. G.} and J.-S. Huang and R. Arendt and P. Barmby and G. Barro and Bell, {E. F.} and R. Bouwens and A. Cattaneo and D. Croton and R. Dav{\'e} and Dunlop, {J. S.} and E. Egami and S. Faber and K. Finlator and Grogin, {N. A.} and P. Guhathakurta and L. Hernquist and Hora, {J. L.} and G. Illingworth and A. Kashlinsky and Koekemoer, {A. M.} and Koo, {D. C.} and I. Labb{\'e} and Y. Li and L. Lin and H. Moseley and K. Nandra and J. Newman and K. Noeske and M. Ouchi and M. Peth and D. Rigopoulou and B. Robertson and V. Sarajedini and L. Simard and Smith, {H. A.} and Z. Wang and R. Wechsler and B. Weiner and G. Wilson and S. Wuyts and T. Yamada and H. Yan",

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doi = "10.1088/0004-637X/769/1/80",

language = "English",

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TY - JOUR

T1 - SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts

AU - Ashby, M. L. N.

AU - Willner, S. P.

AU - Fazio, G. G.

AU - Huang, J.-S.

AU - Arendt, R.

AU - Barmby, P.

AU - Barro, G.

AU - Bell, E. F.

AU - Bouwens, R.

AU - Cattaneo, A.

AU - Croton, D.

AU - Davé, R.

AU - Dunlop, J. S.

AU - Egami, E.

AU - Faber, S.

AU - Finlator, K.

AU - Grogin, N. A.

AU - Guhathakurta, P.

AU - Hernquist, L.

AU - Hora, J. L.

AU - Illingworth, G.

AU - Kashlinsky, A.

AU - Koekemoer, A. M.

AU - Koo, D. C.

AU - Labbé, I.

AU - Li, Y.

AU - Lin, L.

AU - Moseley, H.

AU - Nandra, K.

AU - Newman, J.

AU - Noeske, K.

AU - Ouchi, M.

AU - Peth, M.

AU - Rigopoulou, D.

AU - Robertson, B.

AU - Sarajedini, V.

AU - Simard, L.

AU - Smith, H. A.

AU - Wang, Z.

AU - Wechsler, R.

AU - Weiner, B.

AU - Wilson, G.

AU - Wuyts, S.

AU - Yamada, T.

AU - Yan, H.

PY - 2013/5/20

Y1 - 2013/5/20

N2 - The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalacticscience fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the HubbleDeep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg2 to a depth of 26 AB mag(3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5μm. Because of its uniform depth ofcoverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variancethan a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediateto high redshifts (z = 2–7) with a built-in means of assessing the impact of cosmic variance on the individual fields.Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six-monthintervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. Thispaper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts forthe more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations.Discrete IRAC sources contribute 5.6 ± 1.0 and 4.4 ± 0.8 nW m−2 sr−1 at 3.6 and 4.5μm to the diffuse cosmicinfrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated fromDIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come froma diffuse component.

AB - The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalacticscience fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the HubbleDeep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg2 to a depth of 26 AB mag(3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5μm. Because of its uniform depth ofcoverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variancethan a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediateto high redshifts (z = 2–7) with a built-in means of assessing the impact of cosmic variance on the individual fields.Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six-monthintervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. Thispaper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts forthe more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations.Discrete IRAC sources contribute 5.6 ± 1.0 and 4.4 ± 0.8 nW m−2 sr−1 at 3.6 and 4.5μm to the diffuse cosmicinfrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated fromDIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come froma diffuse component.

KW - galaxies: high redshift

KW - infrared: galaxies

KW - surveys

UR - http://iopscience.iop.org/article/10.1088/0004-637X/769/1/80/meta

U2 - 10.1088/0004-637X/769/1/80

DO - 10.1088/0004-637X/769/1/80

M3 - Article

SN - 0004-637X

VL - 769

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

ER -

SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts

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