Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/30172
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Ashcraft, Teresa A. | en_US |
dc.contributor.author | Windhorst, Rogier A. | en_US |
dc.contributor.author | Jansen, Rolf A. | en_US |
dc.contributor.author | Cohen, Seth H. | en_US |
dc.contributor.author | GRAZIAN, Andrea | en_US |
dc.contributor.author | PARIS, Diego | en_US |
dc.contributor.author | FONTANA, Adriano | en_US |
dc.contributor.author | GIALLONGO, Emanuele | en_US |
dc.contributor.author | SPEZIALI, Roberto | en_US |
dc.contributor.author | TESTA, Vincenzo | en_US |
dc.contributor.author | Boutsia, Konstantina | en_US |
dc.contributor.author | O'Connell, Robert W. | en_US |
dc.contributor.author | Rutkowski, Michael J. | en_US |
dc.contributor.author | Ryan, Russell E. | en_US |
dc.contributor.author | Scarlata, Claudia | en_US |
dc.contributor.author | Weiner, Benjamin | en_US |
dc.date.accessioned | 2021-02-02T15:46:06Z | - |
dc.date.available | 2021-02-02T15:46:06Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-6280 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30172 | - |
dc.description.abstract | We present a study of the trade-off between depth and resolution using a large number of U-band imaging observations in the GOODS-North field from the Large Binocular Camera (LBC) on the Large Binocular Telescope (LBT). Having acquired over 30 hr of data (315 images with 5-6 minutes exposures), we generated multiple image mosaics, starting with the best atmospheric seeing images (FWHM ≲ 0.″8), which constitute ∼10% of the total data set. For subsequent mosaics, we added in data with larger seeing values until the final, deepest mosaic included all images with FWHM ≲ 1.″8 (∼94% of the total data set). From the mosaics, we made object catalogs to compare the optimal-resolution, yet shallower image to the lower-resolution but deeper image. We show that the number counts for both images are ∼90% complete to U <SUB> AB </SUB> ≲ 26 mag. Fainter than U <SUB> AB </SUB> ∼ 27 mag, the object counts from the optimal-resolution image start to drop-off dramatically (90% between U <SUB> AB </SUB> = 27 and 28 mag), while the deepest image with better surface-brightness sensitivity ({μ }<SUB>U</SUB><SUP>{AB</SUP>} ≲ 32 mag arcsec<SUP>-2</SUP>) show a more gradual drop (10% between U <SUB> AB </SUB> ≃ 27 and 28 mag). For the brightest galaxies within the GOODS-N field, structure and clumpy features within the galaxies are more prominent in the optimal-resolution image compared to the deeper mosaics. We conclude that for studies of brighter galaxies and features within them, the optimal-resolution image should be used. However, to fully explore and understand the faintest objects, the deeper imaging with lower resolution are also required. Finally, we find—for 220 brighter galaxies with U <SUB> AB </SUB> ≲ 23 mag—only marginal differences in total flux between the optimal-resolution and lower-resolution light-profiles to {μ }<SUB>U</SUB><SUP>{AB</SUP>} ≲ 32 mag arcsec<SUP>-2</SUP>. In only 10% of the cases are the total-flux differences larger than 0.5 mag. This helps constrain how much flux can be missed from galaxy outskirts, which is important for studies of the Extragalactic Background Light. <P />Based on data acquired using the Large Binocular Telescope (LBT). | en_US |
dc.language.iso | eng | en_US |
dc.title | Ultra-deep Large Binocular Camera U-band Imaging of the GOODS-North Field: Depth Versus Resolution | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1088/1538-3873/aab542 | en_US |
dc.identifier.scopus | 2-s2.0-85057321401 | en_US |
dc.identifier.isi | 000431794900001 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.1088/1538-3873/aab542 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 130 | en_US |
dc.relation.issue | 988 | en_US |
dc.relation.firstpage | 064102 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018PASP..130f4102A | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0002-5688-0663 | - |
crisitem.author.orcid | 0000-0002-7409-8114 | - |
crisitem.author.orcid | 0000-0003-3820-2823 | - |
crisitem.author.orcid | 0000-0003-0734-1273 | - |
crisitem.author.orcid | 0000-0003-3754-387X | - |
crisitem.author.orcid | 0000-0003-1033-1340 | - |
crisitem.journal.journalissn | 0004-6280 | - |
crisitem.journal.ance | E139082 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
File in questo documento:
File | Descrizione | Dimensioni | Formato | |
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2018Ashcraft_arxiv.pdf | postprint | 7.48 MB | Adobe PDF | Visualizza/apri |
Ashcraft_2018_PASP_130_064102.pdf | [Administrators only] | 14.94 MB | Adobe PDF | |
30172-Ashcraft_2018_PASP_130_064102_P01.pdf | Miur | 9.45 MB | Adobe PDF | |
30172-Ashcraft_2018_PASP_130_064102_P02.pdf | Miur | 5.6 MB | Adobe PDF |
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