A z = 5.34 galaxy pair in the Hubble deep field
We present spectrograms of the faint V-drop (V606 = 28.1, I814 = 25.6) galaxy pair HDF 3-951.1 and HDF 3-951.2 obtained at the Keck II Telescope. In a recent study, Fernández-Soto, Lanzetta, and Yahil derive a photometric redshift of zph = 5.28+0.34-0.41 (2 σ) for these galaxies; our integrated spec...
| Main Authors: | , , , , , , , |
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| Format: | Journal article |
| Language: | English |
| Published: |
1998
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| _version_ | 1826268960553697280 |
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| author | Spinrad, H Stern, D Bunker, A Dey, A Lanzetta, K Yahil, A Pascarelle, S Fernandez-Soto, A |
| author_facet | Spinrad, H Stern, D Bunker, A Dey, A Lanzetta, K Yahil, A Pascarelle, S Fernandez-Soto, A |
| author_sort | Spinrad, H |
| collection | OXFORD |
| description | We present spectrograms of the faint V-drop (V606 = 28.1, I814 = 25.6) galaxy pair HDF 3-951.1 and HDF 3-951.2 obtained at the Keck II Telescope. In a recent study, Fernández-Soto, Lanzetta, and Yahil derive a photometric redshift of zph = 5.28+0.34-0.41 (2 σ) for these galaxies; our integrated spectrograms show a large and abrupt discontinuity near 7710 ± 5 Å. This break is almost certainly due to the Lyα forest because its amplitude (1 - fshortv/flongv > 0.87, 95% confidence limit) exceeds any discontinuities observed in stellar or galactic rest-frame optical spectra. The resulting absorption break redshift is z = 5.34 ± 0.01. Optical/near-IR photometry from the HDF yields an exceptionally red (V606 - I814) color, consistent with this large break. A more accurate measure of the continuum depression blueward of Lyα utilizing the imaging photometry yields DA = 0.88. The system as a whole is slightly brighter than L*1500 relative to the z ∼ 3 Lyman break population, and the total star formation rate inferred from the UV continuum is ≈22 h-250 M⊙ yr-1 (q0 = 0.5) assuming the absence of dust extinction. The two individual galaxies are quite small (size scales ≲ 1 h-150 kpc). Thus these galaxies superficially resemble the "building blocks" of Pascarelle and coworkers; if they comprise a gravitationally bound system, the pair will likely merge in a timescale ∼100 Myr. |
| first_indexed | 2024-03-06T21:17:33Z |
| format | Journal article |
| id | oxford-uuid:404e1cc3-65fe-44db-929d-a4aa6d359a9b |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T21:17:33Z |
| publishDate | 1998 |
| record_format | dspace |
| spelling | oxford-uuid:404e1cc3-65fe-44db-929d-a4aa6d359a9b2022-03-26T14:37:08ZA z = 5.34 galaxy pair in the Hubble deep fieldJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:404e1cc3-65fe-44db-929d-a4aa6d359a9bEnglishSymplectic Elements at Oxford1998Spinrad, HStern, DBunker, ADey, ALanzetta, KYahil, APascarelle, SFernandez-Soto, AWe present spectrograms of the faint V-drop (V606 = 28.1, I814 = 25.6) galaxy pair HDF 3-951.1 and HDF 3-951.2 obtained at the Keck II Telescope. In a recent study, Fernández-Soto, Lanzetta, and Yahil derive a photometric redshift of zph = 5.28+0.34-0.41 (2 σ) for these galaxies; our integrated spectrograms show a large and abrupt discontinuity near 7710 ± 5 Å. This break is almost certainly due to the Lyα forest because its amplitude (1 - fshortv/flongv > 0.87, 95% confidence limit) exceeds any discontinuities observed in stellar or galactic rest-frame optical spectra. The resulting absorption break redshift is z = 5.34 ± 0.01. Optical/near-IR photometry from the HDF yields an exceptionally red (V606 - I814) color, consistent with this large break. A more accurate measure of the continuum depression blueward of Lyα utilizing the imaging photometry yields DA = 0.88. The system as a whole is slightly brighter than L*1500 relative to the z ∼ 3 Lyman break population, and the total star formation rate inferred from the UV continuum is ≈22 h-250 M⊙ yr-1 (q0 = 0.5) assuming the absence of dust extinction. The two individual galaxies are quite small (size scales ≲ 1 h-150 kpc). Thus these galaxies superficially resemble the "building blocks" of Pascarelle and coworkers; if they comprise a gravitationally bound system, the pair will likely merge in a timescale ∼100 Myr. |
| spellingShingle | Spinrad, H Stern, D Bunker, A Dey, A Lanzetta, K Yahil, A Pascarelle, S Fernandez-Soto, A A z = 5.34 galaxy pair in the Hubble deep field |
| title | A z = 5.34 galaxy pair in the Hubble deep field |
| title_full | A z = 5.34 galaxy pair in the Hubble deep field |
| title_fullStr | A z = 5.34 galaxy pair in the Hubble deep field |
| title_full_unstemmed | A z = 5.34 galaxy pair in the Hubble deep field |
| title_short | A z = 5.34 galaxy pair in the Hubble deep field |
| title_sort | z 5 34 galaxy pair in the hubble deep field |
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