Observations of the Hubble Deep Field with the Infrared Space Observatory .5. Spectral energy distributions, starburst models and star formation history

被引:219
作者
RowanRobinson, M
Mann, RG
Oliver, SJ
Efstathiou, A
Eaton, N
Goldschmidt, P
Mobasher, B
Serjeant, SBG
Sumner, TJ
Danese, L
Elbaz, D
Franceschini, A
Egami, E
Kontizas, M
Lawrence, A
McMahon, R
NorgaardNielsen, HU
PerezFournon, I
GonzalezSerrano, JI
机构
[1] SISSA, I-34014 TRIESTE, ITALY
[2] SERV ASTROPHYS, F-91191 GIF SUR YVETTE, FRANCE
[3] OSSERV ASTRON PADOVA, I-35122 PADUA, ITALY
[4] MAX PLANCK INST EXTRATERR PHYS, D-37075 GARCHING, GERMANY
[5] NATL OBSERV ATHENS, ASTRON INST, GR-11810 ATHENS, GREECE
[6] UNIV EDINBURGH, ASTRON INST, EDINBURGH EH9 3HJ, MIDLOTHIAN, SCOTLAND
[7] UNIV CAMBRIDGE INST ASTRON, ASTRON INST, CAMBRIDGE CB3 0HA, ENGLAND
[8] DANISH SPACE RES INST, DK-2800 LYNGBY, COPENHAGEN, DENMARK
[9] INST ASTROFIS CANARIAS, E-38200 LA LAGUNA, TENERIFE, SPAIN
[10] INST FIS CANTABRIA, SANTANDER, SPAIN
关键词
stars; formation; galaxies; evolution; starburst; cosmology; observations; infrared;
D O I
10.1093/mnras/289.2.490
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We have modelled the spectral energy distributions of the 13 Hubble Deep Field (HDF) galaxies reliably detected by the Infrared Space Observatory (ISO). For two galaxies the emission detected by ISO is consistent with being starlight or the infrared 'cirrus' in the galaxies. For the remaining II galaxies there is a clear midinfrared excess, which we interpret as emission from dust associated with a strong starburst. 10 of these galaxies are spirals or interacting pairs, while the remaining one is an elliptical with a prominent nucleus and broad emission lines. We give a new discussion of how the star formation rate can be deduced from the far-infrared luminosity, and derive star formation rates for these galaxies of 8-1000 phi M. yr(-1), where phi takes account of the uncertainty in the initial mass function, The HDF galaxies detected by ISO are clearly forming stars at, a prodigious rate compared with nearby normal galaxies, We discuss the implications of our detections for the history of star and heavy element formation in the Universe, Although uncertainties in the calibration, reliability of source detection, associations and starburst models remain, it is clear that dust plays an important role in star formation out to redshift 1 at least.
引用
收藏
页码:490 / 496
页数:7
相关论文
共 30 条
  • [1] Galaxy morphology to I=25 mag in the Hubble Deep Field
    Abraham, RG
    Tanvir, NR
    Santiago, BX
    Ellis, RS
    Glazebrook, K
    vandenBergh, S
    [J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1996, 279 (03) : L47 - &
  • [2] AcostaPulido JA, 1996, ASTRON ASTROPHYS, V315, pL121
  • [3] Aghanim N, 1996, ASTRON ASTROPHYS, V311, P1
  • [4] SPECTRAL EVOLUTION OF STELLAR POPULATIONS USING ISOCHRONE SYNTHESIS
    BRUZUAL, G
    CHARLOT, S
    [J]. ASTROPHYSICAL JOURNAL, 1993, 405 (02) : 538 - 553
  • [5] Redshift clustering in the hubble deep field
    Cohen, JG
    Cowie, LL
    Hogg, DW
    Songaila, A
    Blandford, R
    Hu, EM
    Shopbell, P
    [J]. ASTROPHYSICAL JOURNAL, 1996, 471 (01) : L5 - L9
  • [6] FOMALONT KEB, 1997, APJ, V475, pL5
  • [7] LUMINOSITY EVOLUTION AND DUST EFFECTS IN DISTANT GALAXIES - IMPLICATIONS FOR THE OBSERVABILITY OF THE EARLY EVOLUTIONARY PHASES
    FRANCESCHINI, A
    MAZZEI, P
    DEZOTTI, G
    DANESE, L
    [J]. ASTROPHYSICAL JOURNAL, 1994, 427 (01) : 140 - 154
  • [8] Observations of the Hubble Deep Field with the Infrared Space Observatory .2. Source detection and photometry
    Goldschmidt, P
    Oliver, SJ
    Serjeant, SBG
    Baker, A
    Eaton, N
    Efstathiou, A
    Gruppioni, C
    Mann, RG
    Mobasher, B
    RowanRobinson, M
    Sumner, TJ
    Danese, L
    Elbaz, D
    Franceschini, A
    Egami, E
    Kontizas, M
    Lawrence, A
    McMahon, R
    NorgaardNielsen, HU
    PerezFournon, I
    GonzalezSerrano, JI
    [J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1997, 289 (02) : 465 - 470
  • [9] HOPKINS A, 1997, IN PRESS MNRAS
  • [10] Lilly SJ, 1996, ASTROPHYS J, V460, pL1, DOI 10.1086/309975