2011A&A...532A.152M


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.18CET22:15:10

2011A&A...532A.152M - Astronomy and Astrophysics, volume 532A, 152-152 (2011/8-1)

The Herschel M33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302.

MOOKERJEA B., KRAMER C., BUCHBENDER C., BOQUIEN M., VERLEY S., RELANO M., QUINTANA-LACACI G., AALTO S., BRAINE J., CALZETTI D., COMBES F., GARCIA-BURILLO S., GRATIER P., HENKEL C., ISRAEL F., LORD S., NIKOLA T., ROELLIG M., STACEY G., TABATABAEI F.S., VAN DER TAK F. and VAN DER WERF P.

Abstract (from CDS):

The emission line of [CII] at 158µm is one of the strongest cooling lines of the interstellar medium (ISM) in galaxies. Distinguishing the relative contributions of the different ISM phases to [CII] emission is a major objective of the HerM33es program, a Herschel key project to study the ISM in the nearby spiral galaxy M33. Using PACS, we have mapped the emission of [CII] 158µm, [OI] 63µm, and other FIR lines in a 2'x2' region of the northern spiral arm of M33, centered on the HII region BCLMP302. At the peak of Hα emission, we observed in addition a velocity-resolved [CII] spectrum using HIFI. We use scatterplots to compare these data with PACS 160µm continuum maps, and with maps of CO and HI data, at a common resolution of 12" or 50pc. Maps of Hα and 24µm emission observed with Spitzer are used to estimate the SFR. We created maps of the [CII] and [OI] 63µm emission and detected [NII] 122µm and [NIII] 57µm at individual positions. The [CII] line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between [CII] observed with PACS and CO over the mapped region. There is even less spatial correlation between [CII] and the atomic gas traced by HI. Detailed comparison of the observed intensities towards the HII region with models of photo-ionization and photon-dominated regions, confirms that a significant fraction, 20-30%, of the observed [CII] emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio of [CII] to the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the HII region.

Abstract Copyright:

Journal keyword(s): galaxies: individual: M33 - photon-dominated region (PDR) - HII regions - Local Group - galaxies: ISM - galaxies: star formation

Errata: corrigendum vol.537, art. C3 (2012)

Simbad objects: 19

goto Full paper

goto View the reference in ADS

Number of rows : 19

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11152 1
2 NGC 595 HII 01 33 33.53 +30 41 29.8           ~ 193 0
3 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5231 1
4 IC 142 HII 01 33 55.1 +30 45 22   11.30 14.2     ~ 38 0
5 BCLMP 302 HII 01 34 06.85 +30 47 27.6     14.4     ~ 29 0
6 BCLMP 691 HII 01 34 16.64 +30 51 53.7 14.80 14.63 14.66 14.76 14.76 ~ 30 0
7 NGC 604 HII 01 34 32.1 +30 47 01           ~ 554 0
8 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 330 0
9 NGC 1097 LIN 02 46 19.059 -30 16 29.68 10.46 9.97 9.48 8.72 9.8 ~ 1193 3
10 NGC 1313 G 03 18 16.046 -66 29 53.74   10.06 10.0 9.40 10.4 ~ 615 2
11 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15112 1
12 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1766 1
13 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3867 4
14 M 83 SBG 13 37 00.919 -29 51 56.74 8.85 8.11 7.52 7.21   ~ 2267 2
15 LDN 1721 DNe 16 14 28.1 -18 54 44           ~ 24 0
16 W 49n HII 19 10 13.2 +09 06 12           ~ 421 3
17 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2285 2
18 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 954 0
19 NAME Local Group GrG ~ ~           ~ 7138 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2011A&A...532A.152M and select 'bookmark this link' or equivalent in the popup menu


2021.01.18-22:15:10

© Université de Strasbourg/CNRS

    • Contact