Observations of the Hubble Deep Field with the Infrared Space Observatory - III. Source counts and P(D) analysis

Seb Oliver; Pippa Goldschmidt; A. Franceschini; Steve Serjeant; Andreas Efstathiou; Aprajita Verma; C. Gruppioni; N Eaton; Robert Mann; Bahram Mobasher; Chris Pearson; Michael Rowan-Robinson; Tim Sumner; L. Danese; David Elbaz; E. Egami; M. Kontizas; Andrew Lawrence; Richard McMahon; H. U. Norgaard-Nielsen; I. Perez-Fournon; J. I. Gonzalez-Serrano

doi:10.1093/mnras/289.2.471

Observations of the Hubble Deep Field with the Infrared Space Observatory - III. Source counts and P(D) analysis

Seb Oliver, Pippa Goldschmidt, A. Franceschini, Steve Serjeant, Andreas Efstathiou, Aprajita Verma, C. Gruppioni, N Eaton, Robert Mann, Bahram Mobasher, Chris Pearson, Michael Rowan-Robinson, Tim Sumner, L. Danese, David Elbaz, E. Egami, M. Kontizas, Andrew Lawrence, Richard McMahon, H. U. Norgaard-NielsenI. Perez-Fournon, J. I. Gonzalez-Serrano

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract / Description of output

We present source counts at 6.7 and 15 μm from our maps of the Hubble Deep Field (HDF) region, reaching 38.6 muJy at 6.7 μm and 255 muJy at 15 mum. These are the first ever extragalactic number counts to be presented at 6.7 mum, and are three decades fainter than IRAS at 12 mum. Both source counts and a P(D) analysis suggest that we have reached the Infrared Space Observatory (ISO) confusion limit at 15 mum: this will have important implications for future space missions. These data provide an excellent reference point for other ongoing ISO surveys. A no-evolution model at 15 μm is ruled out at >3sigma, while two models which fit the steep IRAS 60-μm counts are acceptable. This provides important confirmation of the strong evolution seen in IRAS surveys. One of these models can then be ruled out from the 6.7-μm data.

Original language	English
Pages (from-to)	471-481
Journal	Monthly Notices of the Royal Astronomical Society
Volume	289
Issue number	2
DOIs	https://doi.org/10.1093/mnras/289.2.471
Publication status	Published - 1 Aug 1997

Keywords / Materials (for Non-textual outputs)

SURVEYS
GALAXIES: EVOLUTION
GALAXIES: FORMATION
GALAXIES: SEYFERT
GALAXIES: STARBURST
INFRARED: GALAXIES

Access to Document

10.1093/mnras/289.2.471

Cite this

Oliver, S., Goldschmidt, P., Franceschini, A., Serjeant, S., Efstathiou, A., Verma, A., Gruppioni, C., Eaton, N., Mann, R., Mobasher, B., Pearson, C., Rowan-Robinson, M., Sumner, T., Danese, L., Elbaz, D., Egami, E., Kontizas, M., Lawrence, A., McMahon, R., ... Gonzalez-Serrano, J. I. (1997). Observations of the Hubble Deep Field with the Infrared Space Observatory - III. Source counts and P(D) analysis. Monthly Notices of the Royal Astronomical Society, 289(2), 471-481. https://doi.org/10.1093/mnras/289.2.471

@article{929cc4d185a64137ba38e2d735fc3756,

title = "Observations of the Hubble Deep Field with the Infrared Space Observatory - III. Source counts and P(D) analysis",

abstract = "We present source counts at 6.7 and 15 μm from our maps of the Hubble Deep Field (HDF) region, reaching 38.6 muJy at 6.7 μm and 255 muJy at 15 mum. These are the first ever extragalactic number counts to be presented at 6.7 mum, and are three decades fainter than IRAS at 12 mum. Both source counts and a P(D) analysis suggest that we have reached the Infrared Space Observatory (ISO) confusion limit at 15 mum: this will have important implications for future space missions. These data provide an excellent reference point for other ongoing ISO surveys. A no-evolution model at 15 μm is ruled out at >3sigma, while two models which fit the steep IRAS 60-μm counts are acceptable. This provides important confirmation of the strong evolution seen in IRAS surveys. One of these models can then be ruled out from the 6.7-μm data.",

keywords = "SURVEYS, GALAXIES: EVOLUTION, GALAXIES: FORMATION, GALAXIES: SEYFERT, GALAXIES: STARBURST, INFRARED: GALAXIES",

author = "Seb Oliver and Pippa Goldschmidt and A. Franceschini and Steve Serjeant and Andreas Efstathiou and Aprajita Verma and C. Gruppioni and N Eaton and Robert Mann and Bahram Mobasher and Chris Pearson and Michael Rowan-Robinson and Tim Sumner and L. Danese and David Elbaz and E. Egami and M. Kontizas and Andrew Lawrence and Richard McMahon and Norgaard-Nielsen, {H. U.} and I. Perez-Fournon and Gonzalez-Serrano, {J. I.}",

year = "1997",

month = aug,

day = "1",

doi = "10.1093/mnras/289.2.471",

language = "English",

volume = "289",

pages = "471--481",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "2",

}

Oliver, S, Goldschmidt, P, Franceschini, A, Serjeant, S, Efstathiou, A, Verma, A, Gruppioni, C, Eaton, N, Mann, R, Mobasher, B, Pearson, C, Rowan-Robinson, M, Sumner, T, Danese, L, Elbaz, D, Egami, E, Kontizas, M, Lawrence, A, McMahon, R, Norgaard-Nielsen, HU, Perez-Fournon, I & Gonzalez-Serrano, JI 1997, 'Observations of the Hubble Deep Field with the Infrared Space Observatory - III. Source counts and P(D) analysis', Monthly Notices of the Royal Astronomical Society, vol. 289, no. 2, pp. 471-481. https://doi.org/10.1093/mnras/289.2.471

TY - JOUR

T1 - Observations of the Hubble Deep Field with the Infrared Space Observatory - III. Source counts and P(D) analysis

AU - Oliver, Seb

AU - Goldschmidt, Pippa

AU - Franceschini, A.

AU - Serjeant, Steve

AU - Efstathiou, Andreas

AU - Verma, Aprajita

AU - Gruppioni, C.

AU - Eaton, N

AU - Mann, Robert

AU - Mobasher, Bahram

AU - Pearson, Chris

AU - Rowan-Robinson, Michael

AU - Sumner, Tim

AU - Danese, L.

AU - Elbaz, David

AU - Egami, E.

AU - Kontizas, M.

AU - Lawrence, Andrew

AU - McMahon, Richard

AU - Norgaard-Nielsen, H. U.

AU - Perez-Fournon, I.

AU - Gonzalez-Serrano, J. I.

PY - 1997/8/1

Y1 - 1997/8/1

N2 - We present source counts at 6.7 and 15 μm from our maps of the Hubble Deep Field (HDF) region, reaching 38.6 muJy at 6.7 μm and 255 muJy at 15 mum. These are the first ever extragalactic number counts to be presented at 6.7 mum, and are three decades fainter than IRAS at 12 mum. Both source counts and a P(D) analysis suggest that we have reached the Infrared Space Observatory (ISO) confusion limit at 15 mum: this will have important implications for future space missions. These data provide an excellent reference point for other ongoing ISO surveys. A no-evolution model at 15 μm is ruled out at >3sigma, while two models which fit the steep IRAS 60-μm counts are acceptable. This provides important confirmation of the strong evolution seen in IRAS surveys. One of these models can then be ruled out from the 6.7-μm data.

AB - We present source counts at 6.7 and 15 μm from our maps of the Hubble Deep Field (HDF) region, reaching 38.6 muJy at 6.7 μm and 255 muJy at 15 mum. These are the first ever extragalactic number counts to be presented at 6.7 mum, and are three decades fainter than IRAS at 12 mum. Both source counts and a P(D) analysis suggest that we have reached the Infrared Space Observatory (ISO) confusion limit at 15 mum: this will have important implications for future space missions. These data provide an excellent reference point for other ongoing ISO surveys. A no-evolution model at 15 μm is ruled out at >3sigma, while two models which fit the steep IRAS 60-μm counts are acceptable. This provides important confirmation of the strong evolution seen in IRAS surveys. One of these models can then be ruled out from the 6.7-μm data.

KW - SURVEYS

KW - GALAXIES: EVOLUTION

KW - GALAXIES: FORMATION

KW - GALAXIES: SEYFERT

KW - GALAXIES: STARBURST

KW - INFRARED: GALAXIES

U2 - 10.1093/mnras/289.2.471

DO - 10.1093/mnras/289.2.471

M3 - Article

SN - 0035-8711

VL - 289

SP - 471

EP - 481

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

Observations of the Hubble Deep Field with the Infrared Space Observatory - III. Source counts and P(D) analysis

Abstract / Description of output

Keywords / Materials (for Non-textual outputs)

Access to Document

Fingerprint

Cite this