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Green, Joel D.,Evans II, Neal J.,Jørgensen, Jes K.,Herczeg, Gregory J.,Kristensen, Lars E.,Lee, Jeong-Eun,Dionatos, Odysseas,Yildiz, Umut A.,Salyk, Colette,Meeus, Gwendolyn,Bouwman, Jeroen,Visser, Ruu IOP Publishing 2013 The Astrophysical journal Vol.770 No.2
<P>We present 50-210 mu m spectral scans of 30 Class 0/I protostellar sources, obtained with Herschel-PACS, and 0.5-1000 mu m spectral energy distributions, as part of the Dust, Ice, and Gas in Time Key Program. Some sources exhibit up to 75 H2O lines ranging in excitation energy from 100 to 2000 K, 12 transitions of OH, and CO rotational lines ranging from J = 14 -> 13 up to J = 40 -> 39. [O I] is detected in all but one source in the entire sample; among the sources with detectable [O I] are two very low luminosity objects. The mean 63/145 mu m [O I] flux ratio is 17.2 +/- 9.2. The [O I] 63 mu m line correlates with L-bol, but not with the time-averaged outflow rate derived from low-J CO maps. [C II] emission is in general not local to the source. The sample L-bol increased by 1.25 (1.06) and T-bol decreased to 0.96 (0.96) of mean (median) values with the inclusion of the Herschel data. Most CO rotational diagrams are characterized by two optically thin components (< N > = ( 0.70 +/- 1.12) x 10(49) total particles). N-CO correlates strongly with L-bol, but neither T-rot nor N-CO(warm)/N-CO(hot) correlates with L-bol, suggesting that the total excited gas is related to the current source luminosity, but that the excitation is primarily determined by the physics of the interaction (e.g., UV-heating/shocks). Rotational temperatures for H2O (< T-rot > = 194 +/- 85 K) and OH (< T-rot > = 183 +/- 117 K) are generally lower than for CO, and much of the scatter in the observations about the best fit is attributed to differences in excitation conditions and optical depths among the detected lines.</P>
L1448-MM OBSERVATIONS BY THE <i>HERSCHEL</i> KEY PROGRAM, “DUST, ICE, AND GAS IN TIME” (DIGIT)
Lee, Jinhee,Lee, Jeong-Eun,Lee, Seokho,Green, Joel. D.,Evans II, Neal J.,Choi, Minho,Kristensen, Lars,Dionatos, Odysseas,Jørgensen, Jes K. IOP Publishing 2013 The Astrophysical journal, Supplement series Vol.209 No.1
CO in Protostars (COPS): <i>Herschel</i>-SPIRE Spectroscopy of Embedded Protostars
Yang, Yao-Lun,Green, Joel D.,Evans II, Neal J.,Lee, Jeong-Eun,Jørgensen, Jes K.,Kristensen, Lars E.,Mottram, Joseph C.,Herczeg, Gregory,Karska, Agata,Dionatos, Odysseas,Bergin, Edwin A.,Bouwman, Jeroe American Astronomical Society 2018 The Astrophysical journal Vol.860 No.2
<P>We present full spectral scans from 200 to 670. mu m of 26 Class 0+I protostellar sources obtained with Herschel-SPIRE as part of the 'COPS-SPIRE' Open Time program, complementary to the DIGIT and WISH Key Programs. Based on our nearly continuous, line-free spectra from 200 to 670. mu m, the calculated bolometric luminosities (L-bol) increase by 50%. on average, and the bolometric temperatures (T-bol) decrease by 10%. on average, in comparison with the measurements without Herschel. Fifteen protostars have the same class using Tbol and L-bol/L-smm. We identify rotational transitions of CO lines from J = 4 -> 3to J = 13 -> 12, along with emission lines of (CO)-C-13, HCO+, H2O, and [C I]. The ratios of (CO)-C-12 to (CO)-C-13 indicate that (CO)-C-12 emission remains optically thick for J(up) < 13. We fit up to four components of temperature from the rotational diagram with flexible break points to separate the components. The distribution of rotational temperatures shows a primary population around 100 K with a secondary population at similar to 350 K. We quantify the correlations of each line pair found in our data set and find that the strength of the correlation of CO lines decreases as the difference between J levels between two CO lines increases. The multiple origins of CO emission previously revealed by velocity-resolved profiles are consistent with this smooth distribution if each physical component contributes to a wide range of CO lines with significant overlap in the CO ladder. We investigate the spatial extent of CO emission and find that the morphology is more centrally peaked and less bipolar at high-J lines. We find the CO emission observed with SPIRE related to outflows, which consists of two components, the entrained gas and shocked gas, as revealed by our rotational diagram analysis, as well as the studies with velocity-resolved CO emission.</P>