FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W1489770520> ?p ?o ?g. }

• W1489770520 endingPage "3054" @default.
• W1489770520 startingPage "3041" @default.
• W1489770520 abstract "We present near-infrared observations of the active galactic nuclei (AGNs) and star-forming objects in the field of the radio galaxy 53W002 at z = 2.39. The star-forming objects are of special interest as candidate protogalactic objects. The 1.1–2.2 μm passbands sample the emitted-optical range at this redshift, providing new diagnostics of the structure, metal abundance, and age of the members of this grouping originally selected through Lyα emission. The star-forming objects are uniformly very blue in continuum slope, which fits with the strong Lyα emission in indicating metal abundances that are less than half solar; some are as blue as the most metal-poor local objects. They fall in a range of luminosity and metallicity that is not populated by local objects, indicating a shorter star-forming history at this early epoch. The best local analogs, such as Mrk 66 and 357, either have several times lower luminosity at comparable [O/H] or significantly higher [O/H] for comparable luminosity. Spectroscopy from the Near-Infrared Camera and Multi-Object Spectrometer yields detections of [O III] emission for two objects and interesting [O III] and Hβ limits for the rest, augmented by Hα limits from Infrared Telescope Facility imaging. These data are satisfied by model stellar populations that have been forming stars for the last 2–5 × 106 yr before z = 2.39. We do not see evidence for older preexisting stellar populations, either in the broadband colors or as redder halos in which the star-forming regions are imbedded. These results suggest that the compact star-forming objects we see at z = 2.0–2.5 are indeed early stages in the building of galaxies rather than transient star-forming events in larger pre-existing dynamical systems. The results also allow an alternative scheme, in which these are low-mass systems that are blowing winds rather than self-enriching, in which case they should fade rapidly with cosmic epoch. For the three prominent AGNs at z = 2.39, Hα and [O III] emission were measured. Unlike the fainter star-forming objects, their line ratios (specifically Lyα/Hα) show metallicities just as high as in nearby systems. If the AGNs occur in those systems that started with the highest density and began active star formation before the less massive surrounding objects, they will have higher metallicity (as we see in their emitted-ultraviolet line ratios). The ionization cones seen prominently in Lyα also appear in [O III] and Hα, with a role for continuum reflection in some cases as well. The contrast between the AGNs and fainter star-forming objects can be broadly accommodated in a hierarchical formation picture, although there are still important unknowns as to the fate of the star-forming objects." @default.
• W1489770520 created "2016-06-24" @default.
• W1489770520 creator A5007359651 @default.
• W1489770520 creator A5020647140 @default.
• W1489770520 creator A5034653116 @default.
• W1489770520 creator A5041668884 @default.
• W1489770520 creator A5077171074 @default.
• W1489770520 date "2002-06-01" @default.
• W1489770520 modified "2023-09-23" @default.
• W1489770520 title "Active Nuclei and Star-forming Objects at [ITAL][CLC]z[/CLC][/ITAL] ] 2: Metallicities, Winds, and Formation Histories" @default.
• W1489770520 cites W1483195640 @default.
• W1489770520 cites W1534174676 @default.
• W1489770520 cites W1665422179 @default.
• W1489770520 cites W1969070606 @default.
• W1489770520 cites W1971191206 @default.
• W1489770520 cites W1974174849 @default.
• W1489770520 cites W1976416986 @default.
• W1489770520 cites W1982222124 @default.
• W1489770520 cites W1985933276 @default.
• W1489770520 cites W1990726182 @default.
• W1489770520 cites W2006360799 @default.
• W1489770520 cites W2010845260 @default.
• W1489770520 cites W2013426076 @default.
• W1489770520 cites W2020893016 @default.
• W1489770520 cites W2026818795 @default.
• W1489770520 cites W2029438261 @default.
• W1489770520 cites W2031244266 @default.
• W1489770520 cites W2033203361 @default.
• W1489770520 cites W2034133576 @default.
• W1489770520 cites W2035775205 @default.
• W1489770520 cites W2043130408 @default.
• W1489770520 cites W2047267722 @default.
• W1489770520 cites W2051524665 @default.
• W1489770520 cites W2058672304 @default.
• W1489770520 cites W2059511259 @default.
• W1489770520 cites W2067698390 @default.
• W1489770520 cites W2070696493 @default.
• W1489770520 cites W2079683183 @default.
• W1489770520 cites W2083609040 @default.
• W1489770520 cites W2087392640 @default.
• W1489770520 cites W2108386285 @default.
• W1489770520 cites W2124181276 @default.
• W1489770520 cites W2140887005 @default.
• W1489770520 cites W2145225754 @default.
• W1489770520 cites W3012511726 @default.
• W1489770520 cites W3100420956 @default.
• W1489770520 cites W3104715447 @default.
• W1489770520 cites W3105349666 @default.
• W1489770520 cites W3105572495 @default.
• W1489770520 cites W3106327613 @default.
• W1489770520 cites W3106512278 @default.
• W1489770520 cites W3122032508 @default.
• W1489770520 cites W3123921119 @default.
• W1489770520 cites W3124401234 @default.
• W1489770520 doi "https://doi.org/10.1086/340696" @default.
• W1489770520 hasPublicationYear "2002" @default.
• W1489770520 type Work @default.
• W1489770520 sameAs 1489770520 @default.
• W1489770520 citedByCount "15" @default.
• W1489770520 countsByYear W14897705202012 @default.
• W1489770520 countsByYear W14897705202013 @default.
• W1489770520 countsByYear W14897705202016 @default.
• W1489770520 countsByYear W14897705202017 @default.
• W1489770520 crossrefType "journal-article" @default.
• W1489770520 hasAuthorship W1489770520A5007359651 @default.
• W1489770520 hasAuthorship W1489770520A5020647140 @default.
• W1489770520 hasAuthorship W1489770520A5034653116 @default.
• W1489770520 hasAuthorship W1489770520A5041668884 @default.
• W1489770520 hasAuthorship W1489770520A5077171074 @default.
• W1489770520 hasBestOaLocation W14897705201 @default.
• W1489770520 hasConcept C121332964 @default.
• W1489770520 hasConcept C12287442 @default.
• W1489770520 hasConcept C125857072 @default.
• W1489770520 hasConcept C1276947 @default.
• W1489770520 hasConcept C150846664 @default.
• W1489770520 hasConcept C33024259 @default.
• W1489770520 hasConcept C43481613 @default.
• W1489770520 hasConcept C44870925 @default.
• W1489770520 hasConcept C98444146 @default.
• W1489770520 hasConcept C99465377 @default.
• W1489770520 hasConceptScore W1489770520C121332964 @default.
• W1489770520 hasConceptScore W1489770520C12287442 @default.
• W1489770520 hasConceptScore W1489770520C125857072 @default.
• W1489770520 hasConceptScore W1489770520C1276947 @default.
• W1489770520 hasConceptScore W1489770520C150846664 @default.
• W1489770520 hasConceptScore W1489770520C33024259 @default.
• W1489770520 hasConceptScore W1489770520C43481613 @default.
• W1489770520 hasConceptScore W1489770520C44870925 @default.
• W1489770520 hasConceptScore W1489770520C98444146 @default.
• W1489770520 hasConceptScore W1489770520C99465377 @default.
• W1489770520 hasIssue "6" @default.
• W1489770520 hasLocation W14897705201 @default.
• W1489770520 hasOpenAccess W1489770520 @default.
• W1489770520 hasPrimaryLocation W14897705201 @default.
• W1489770520 hasRelatedWork W1788650297 @default.
• W1489770520 hasRelatedWork W2047108234 @default.
• W1489770520 hasRelatedWork W2047342598 @default.
• W1489770520 hasRelatedWork W2137397364 @default.

• next