FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3004964926> ?p ?o ?g. }

• W3004964926 endingPage "162" @default.
• W3004964926 startingPage "162" @default.
• W3004964926 abstract "We report Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO $(8-7)$, $(9-8)$, $rm H_{2}O (2_{0,2}-1_{1,1})$ and $rm OH^{+} (1_{1}-0_{1})$ and NOrthern Extended Millimeter Array (NOEMA) observations of CO $(5-4)$, $(6-5)$, $(12-11)$ and $(13-12)$ towards the $z = 6.003$ quasar SDSS J231038.88+185519.7, aiming to probe the physical conditions of the molecular gas content of this source. We present the best sampled CO spectral line energy distribution (SLED) at $z = 6.003$, and analyzed it with the radiative transfer code MOLPOP-CEP. Fitting the CO SLED to a one-component model indicates a kinetic temperature $T_{rm kin} = 228 rm K$, molecular gas density $log (n(rm H_{2})/rm cm^{-3}$ )=4.75, and CO column density $log(N(rm CO)/rm cm^{-2}) =17.5$, although a two-component model better fits the data. In either case, the CO SLED is dominated by a warm and dense component. Compared to samples of local (Ultra) Luminous Infrared Galaxies ((U)LIRGs), starburst galaxies and high redshift Submillimeter Galaxies (SMGs), J2310+1855 exhibits higher CO excitation at ($J geq 8$), like other high redshift quasars. The high CO excitation, together with the enhanced $L_{rm H_{2}O}/ L_{IR} $, $L_{rm H_{2}O}/ L_{CO} $ and $L_{OH^{+}}/L_{rm H_{2}O} $ ratios, suggests that besides the UV radiation from young massive stars, other mechanisms such as shocks, cosmic rays and X-rays might also be responsible for the heating and ionization of the molecular gas. In the nuclear region probed by the molecular emissions lines, any of these mechanisms might be present due to the powerful quasar and the starburst activity." @default.
• W3004964926 created "2020-02-14" @default.
• W3004964926 creator A5007660640 @default.
• W3004964926 creator A5009520028 @default.
• W3004964926 creator A5018789920 @default.
• W3004964926 creator A5025532100 @default.
• W3004964926 creator A5026512679 @default.
• W3004964926 creator A5026859057 @default.
• W3004964926 creator A5030109075 @default.
• W3004964926 creator A5036551344 @default.
• W3004964926 creator A5037268871 @default.
• W3004964926 creator A5051640991 @default.
• W3004964926 creator A5057320280 @default.
• W3004964926 creator A5069209748 @default.
• W3004964926 creator A5080922192 @default.
• W3004964926 creator A5081663262 @default.
• W3004964926 creator A5083465619 @default.
• W3004964926 creator A5087365236 @default.
• W3004964926 creator A5090206203 @default.
• W3004964926 date "2020-02-04" @default.
• W3004964926 modified "2023-10-09" @default.
• W3004964926 title "Probing the Full CO Spectral Line Energy Distribution (SLED) in the Nuclear Region of a Quasar-starburst System at <i>z</i> = 6.003" @default.
• W3004964926 cites W1628272566 @default.
• W3004964926 cites W1818803249 @default.
• W3004964926 cites W1921256341 @default.
• W3004964926 cites W1967440647 @default.
• W3004964926 cites W1972700440 @default.
• W3004964926 cites W1979253784 @default.
• W3004964926 cites W1980265098 @default.
• W3004964926 cites W1980459591 @default.
• W3004964926 cites W1984204014 @default.
• W3004964926 cites W2000083902 @default.
• W3004964926 cites W2001852248 @default.
• W3004964926 cites W2021227168 @default.
• W3004964926 cites W2023012094 @default.
• W3004964926 cites W2025152207 @default.
• W3004964926 cites W2031615933 @default.
• W3004964926 cites W2034783616 @default.
• W3004964926 cites W2037744399 @default.
• W3004964926 cites W2040503929 @default.
• W3004964926 cites W2042897921 @default.
• W3004964926 cites W2043280563 @default.
• W3004964926 cites W2047156688 @default.
• W3004964926 cites W2054675898 @default.
• W3004964926 cites W2059309055 @default.
• W3004964926 cites W2074565984 @default.
• W3004964926 cites W2075593391 @default.
• W3004964926 cites W2076606631 @default.
• W3004964926 cites W2089159147 @default.
• W3004964926 cites W2094504621 @default.
• W3004964926 cites W2101687185 @default.
• W3004964926 cites W2102308434 @default.
• W3004964926 cites W2104291306 @default.
• W3004964926 cites W2115547515 @default.
• W3004964926 cites W2129932593 @default.
• W3004964926 cites W2130425957 @default.
• W3004964926 cites W2135691350 @default.
• W3004964926 cites W2140638199 @default.
• W3004964926 cites W2141105013 @default.
• W3004964926 cites W2149332780 @default.
• W3004964926 cites W2169817004 @default.
• W3004964926 cites W2485353633 @default.
• W3004964926 cites W2528174261 @default.
• W3004964926 cites W2534491916 @default.
• W3004964926 cites W2562907507 @default.
• W3004964926 cites W2618742974 @default.
• W3004964926 cites W2735068436 @default.
• W3004964926 cites W2744260194 @default.
• W3004964926 cites W2792435769 @default.
• W3004964926 cites W2806314189 @default.
• W3004964926 cites W2885422816 @default.
• W3004964926 cites W2902191872 @default.
• W3004964926 cites W2918652883 @default.
• W3004964926 cites W2930314552 @default.
• W3004964926 cites W2947851259 @default.
• W3004964926 cites W2951911578 @default.
• W3004964926 cites W2964210593 @default.
• W3004964926 cites W2981762500 @default.
• W3004964926 cites W2994936490 @default.
• W3004964926 cites W3021013694 @default.
• W3004964926 cites W3098285984 @default.
• W3004964926 cites W3098619061 @default.
• W3004964926 cites W3098667503 @default.
• W3004964926 cites W3098981228 @default.
• W3004964926 cites W3099040726 @default.
• W3004964926 cites W3099196797 @default.
• W3004964926 cites W3100412167 @default.
• W3004964926 cites W3100497253 @default.
• W3004964926 cites W3100805745 @default.
• W3004964926 cites W3100830970 @default.
• W3004964926 cites W3101165878 @default.
• W3004964926 cites W3102014803 @default.
• W3004964926 cites W3102307902 @default.
• W3004964926 cites W3102318274 @default.
• W3004964926 cites W3102400022 @default.
• W3004964926 cites W3102697983 @default.
• W3004964926 cites W3102804094 @default.
• W3004964926 cites W3103137868 @default.

• next