Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy
We present Keck Low Resolution Imaging Spectrometer spectroscopy along with Near-Infrared Camera and Multiobject Spectrometer (NICMOS) F110W (∼J) and F160W (∼H) images of the galaxy HDF 4-473.0 in the Hubble Deep Field (HDF), with a detection of an emission line consistent with Lyα at a redshift of...
| Main Authors: | , , , , , , |
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| Format: | Journal article |
| Language: | English |
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Institute of Physics Publishing
1998
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| _version_ | 1826292290593751040 |
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| author | Weymann, R Stern, D Bunker, A Spinrad, H Chaffee, F Thompson, R Storrie-Lombardi, L |
| author_facet | Weymann, R Stern, D Bunker, A Spinrad, H Chaffee, F Thompson, R Storrie-Lombardi, L |
| author_sort | Weymann, R |
| collection | OXFORD |
| description | We present Keck Low Resolution Imaging Spectrometer spectroscopy along with Near-Infrared Camera and Multiobject Spectrometer (NICMOS) F110W (∼J) and F160W (∼H) images of the galaxy HDF 4-473.0 in the Hubble Deep Field (HDF), with a detection of an emission line consistent with Lyα at a redshift of z = 5.60. Attention to this object as a high-redshift galaxy was first drawn by Lanzetta, Yahil, and Fernandez-Soto and appeared in their initial list of galaxies with redshifts estimated from the Wide Field Planetary Camera 2 (WFPC2) HDF photometry. It was selected by us for spectroscopic observation, along with others in the HDF, on the basis of the NICMOS F110W and F160W and WFPC2 photometry. ForH0 = 65 km s-1 Mpc-1 and q0 = 0.125, the use of simple evolutionary models along with the F814W (∼I), F110W, and F160W magnitudes allow us to estimate the star formation rate (∼13 M⊙ yr-1). The colors suggest a reddening of E(B - V) ∼ 0.06. The measured flux in the Lyα line is approximately 1.0 × 10-17 ergs cm-2 s-1, and the rest-frame equivalent width, correcting for the absorption caused by intervening H I, is ∼90 Å. The galaxy is compact and regular, but resolved, with an observed FWHM of ∼0″.44. Simple evolutionary models can accurately reproduce the colors, and these models predict the Lyα flux to within a factor of 2. Using this object as a template shifted to higher redshifts, we calculate the magnitudes through the F814W and two NICMOS passbands for galaxies at redshifts 6 < z < 10. © 1998. The American Astronomical Socicly. All rights reserved. |
| first_indexed | 2024-03-07T03:12:25Z |
| format | Journal article |
| id | oxford-uuid:b4a2f9d4-4ebf-47e5-b9c4-a4f41c0b0cc0 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T03:12:25Z |
| publishDate | 1998 |
| publisher | Institute of Physics Publishing |
| record_format | dspace |
| spelling | oxford-uuid:b4a2f9d4-4ebf-47e5-b9c4-a4f41c0b0cc02022-03-27T04:27:40ZKeck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxyJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:b4a2f9d4-4ebf-47e5-b9c4-a4f41c0b0cc0EnglishSymplectic Elements at OxfordInstitute of Physics Publishing1998Weymann, RStern, DBunker, ASpinrad, HChaffee, FThompson, RStorrie-Lombardi, LWe present Keck Low Resolution Imaging Spectrometer spectroscopy along with Near-Infrared Camera and Multiobject Spectrometer (NICMOS) F110W (∼J) and F160W (∼H) images of the galaxy HDF 4-473.0 in the Hubble Deep Field (HDF), with a detection of an emission line consistent with Lyα at a redshift of z = 5.60. Attention to this object as a high-redshift galaxy was first drawn by Lanzetta, Yahil, and Fernandez-Soto and appeared in their initial list of galaxies with redshifts estimated from the Wide Field Planetary Camera 2 (WFPC2) HDF photometry. It was selected by us for spectroscopic observation, along with others in the HDF, on the basis of the NICMOS F110W and F160W and WFPC2 photometry. ForH0 = 65 km s-1 Mpc-1 and q0 = 0.125, the use of simple evolutionary models along with the F814W (∼I), F110W, and F160W magnitudes allow us to estimate the star formation rate (∼13 M⊙ yr-1). The colors suggest a reddening of E(B - V) ∼ 0.06. The measured flux in the Lyα line is approximately 1.0 × 10-17 ergs cm-2 s-1, and the rest-frame equivalent width, correcting for the absorption caused by intervening H I, is ∼90 Å. The galaxy is compact and regular, but resolved, with an observed FWHM of ∼0″.44. Simple evolutionary models can accurately reproduce the colors, and these models predict the Lyα flux to within a factor of 2. Using this object as a template shifted to higher redshifts, we calculate the magnitudes through the F814W and two NICMOS passbands for galaxies at redshifts 6 < z < 10. © 1998. The American Astronomical Socicly. All rights reserved. |
| spellingShingle | Weymann, R Stern, D Bunker, A Spinrad, H Chaffee, F Thompson, R Storrie-Lombardi, L Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy |
| title | Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy |
| title_full | Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy |
| title_fullStr | Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy |
| title_full_unstemmed | Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy |
| title_short | Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy |
| title_sort | keck spectroscopy and nicmos photometry of a redshift z 5 60 galaxy |
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