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

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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 deg 2 to a depth of 26 AB mag (3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 μm. 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 4.5 μm 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 languageEnglish (US)
Article number80
JournalAstrophysical Journal
Volume769
Issue number1
DOIs
StatePublished - May 20 2013

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survey design
photometry
cameras
galaxies
faint objects
data products
field survey
strip

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ashby, M. L. N., Willner, S. P., Fazio, G. G., Huang, J. S., Arendt, R., Barmby, P., ... Yan, H. (2013). Seds: The spitzer extended deep survey. Survey design, photometry, and deep irac source counts. Astrophysical Journal, 769(1), [80]. https://doi.org/10.1088/0004-637X/769/1/80
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. ; Hora, J. L. ; Illingworth, G. ; Kashlinsky, A. ; Koekemoer, A. M. ; Koo, D. C. ; 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, H. A. ; Wang, Z. ; Wechsler, R. ; Weiner, B. ; Wilson, G. ; Wuyts, S. ; Yamada, T. ; Yan, H. / Seds : The spitzer extended deep survey. Survey design, photometry, and deep irac source counts. In: Astrophysical Journal. 2013 ; Vol. 769, No. 1.
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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 deg 2 to a depth of 26 AB mag (3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 μm. 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 4.5 μm 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.",
author = "Ashby, {M. L.N.} and Willner, {S. P.} and Fazio, {G. G.} and Huang, {J. S.} 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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Ashby, MLN, Willner, SP, Fazio, GG, Huang, JS, 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, 80. https://doi.org/10.1088/0004-637X/769/1/80

Seds : The spitzer extended deep survey. Survey design, photometry, and deep irac source counts. / 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.; Hora, J. L.; Illingworth, G.; Kashlinsky, A.; Koekemoer, A. M.; Koo, D. C.; 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, H. A.; Wang, Z.; Wechsler, R.; Weiner, B.; Wilson, G.; Wuyts, S.; Yamada, T.; Yan, H.

In: Astrophysical Journal, Vol. 769, No. 1, 80, 20.05.2013.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Seds

T2 - 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 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 deg 2 to a depth of 26 AB mag (3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 μm. 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 4.5 μm 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.

AB - 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 deg 2 to a depth of 26 AB mag (3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 μm. 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 4.5 μm 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.

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