- ttf a écrit:
- Toutes des diffuses... La polémique évolutive n'est pas éteinte...
Tout à fait !!!
ALMA surveyed the Hubble Ultra Deep Field, uncovering new details of the star-forming history of the Universe. This animated GIF reveals one such galaxy (orange), rich in carbon monoxide, showing it is primed for star formation. The blue features are galaxies imaged by Hubble. Credit: B. Saxton (NRAO/AUI/NSF); ALMA (ESO/NAOJ/NRAO); NASA/ESA Hubble | Download image22 September 2016ALMA Explores the Hubble Ultra Deep Field:
Uncovers Insights into 'Golden Age' of Galaxy Formation
An international team of astronomers using the Atacama Large Millimeter/submillimeter Array (ALMA) has explored the same distant corner of the universe first revealed in the iconic image of the Hubble Ultra Deep Field (HUDF).
The new ALMA observations, which are significantly deeper and sharper than previous surveys at millimeter wavelengths, trace the previously unknown abundance of star-forming gas at different points in time, providing new insights into the "Golden Age" of galaxy formation approximately 10 billion years ago.
The researchers presented their findings today at the Half a Decade of ALMA conference in Palm Springs, California. The results also are accepted for publication in a series of seven scientific papers appearing in the
Astrophysical Journal.
https://public.nrao.edu/news/pressreleases/2016-alma-hudf
These cutout images are from a combination of a background picture taken by the NASA/ESA Hubble Space Telescope (blue/green) with a new very deep ALMA view of the field (orange, marked with circles). All the objects that ALMA sees appear to be massive star-forming galaxies. This image is based on the ALMA survey by J. Dunlop and colleagues, covering the full HUDF area. Credit: ALMA (ESO/NAOJ/NRAO)/NASA/ESA/J. Dunlop et al. and S. Beckwith (STScI) and the HUDF Team.
THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: IMPLICATIONS FOR SPECTRAL LINE INTENSITY MAPPING AT MILLIMETER WAVELENGTHS AND CMB SPECTRAL DISTORTIONS
http://arxiv.org/pdf/1607.06773v3.pdf
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: MOLECULAR GAS RESERVOIRS IN HIGH{REDSHIFT GALAXIES
https://arxiv.org/pdf/1607.06771v2.pdf
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CO LUMINOSITY FUNCTIONS AND THE EVOLUTION OF THE COSMIC DENSITY OF MOLECULAR GAS
https://arxiv.org/pdf/1607.06770v2.pdf
THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CONTINUUM NUMBER COUNTS, RESOLVED 1.2-MM EXTRAGALACTIC BACKGROUND, AND PROPERTIES OF THE FAINTEST DUSTY STAR FORMING GALAXIES
https://arxiv.org/pdf/1607.06769v2.pdf
ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Survey Description
Authors: Fabian Walter, Roberto Decarli, Manuel Aravena, Chris Carilli, Rychard Bouwens, Elisabete da Cunha, Emanuele Daddi, R. J. Ivison, Dominik Riechers, Ian Smail, Mark Swinbank, Axel Weiss, Timo Anguita, Roberto Assef, Roland Bacon, Franz Bauer, Eric F. Bell, Frank Bertoldi, Scott Chapman, Luis Colina, Paulo C. Cortes, Pierre Cox, Mark Dickinson, David Elbaz, Jorge Gónzalez-López, Edo Ibar, Hanae Inami, Leopoldo Infante, Jacqueline Hodge, Alex Karim, Olivier Le Fevre, Benjamin Magnelli, Roberto Neri, Pascal Oesch, Kazuaki Ota, Gergö Popping, Hans-Walter Rix, Mark Sargent, Kartik Sheth, Arjen van der Wel, Paul van der Werf, Jeff Wagg
(Submitted on 22 Jul 2016)
- Citation :
- Abstract: We present the rationale for and the observational description of ASPECS: The ALMA SPECtroscopic Survey in the Hubble Ultra-Deep Field (UDF), the cosmological deep field that has the deepest multi-wavelength data available. Our overarching goal is to obtain an unbiased census of molecular gas and dust continuum emission in high-redshift (z> 0.5) galaxies. The ∼ 1 [size=16]′ [/size] region covered within the UDF was chosen to overlap with the deepest available imaging from HST. Our ALMA observations consist of full frequency scans in band 3 (84-115 GHz) and band 6 (212-272 GHz) at approximately uniform line sensitivity (L [size=16]′ CO ∼ [/size] 2× 10 [size=16]9 [/size] K km/s pc [size=16]2 [/size] ), and continuum noise levels of 3.8 μ Jy beam [size=11]−1 [/size] and 12.7 μ Jy beam [size=11]−1 [/size] , respectively. The molecular surveys cover the different rotational transitions of the CO molecule, leading to essentially full redshift coverage. The [CII] emission line is also covered at redshifts 6.0<z<8.0 . We present a customized algorithm to identify line candidates in the molecular line scans, and quantify our ability to recover artificial sources from our data. Based on whether multiple CO lines are detected, and whether optical spectroscopic redshifts as well as optical counterparts exist, we constrain the most likely line identification. We report 10 (11) CO line candidates in the 3mm (1mm) band, and our statistical analysis shows that < 4 of these (in each band) are likely spurious. Less than 1/3 of the total CO flux in the low-J CO line candidates are from sources that are not associated with an optical/NIR counterpart. We also present continuum maps of both the band 3 and band 6 observations. The data presented here form the basis of a number of dedicated studies that are presented in subsequent papers.
| Comments: |
| Subjects: | Astrophysics of Galaxies (astro-ph.GA) |
| Cite as: | arXiv:1607.06768 [astro-ph.GA] |
| | (or arXiv:1607.06768v1 [astro-ph.GA] for this version) |
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