Spatially-Resolved Dense Molecular Gas and Star Formation Rate in M51
| hal.structure.identifier | Department of mathematics | |
| dc.contributor.author | CHEN, Hao, | |
| dc.contributor.author | GAO, Yu, | |
| hal.structure.identifier | FORMATION STELLAIRE 2015 | |
| dc.contributor.author | BRAINE, J. | |
| dc.contributor.author | GU, Qiusheng, | |
| dc.date.issued | 2015-07 | |
| dc.identifier.issn | 0004-637X | |
| dc.description.abstractEn | We present the spatially-resolved observations of HCN J = 1 -- 0 emission in the nearby spiral galaxy M51 using the IRAM 30 m telescope. The HCN map covers an extent of $4\arcmin\times5\arcmin$ with spatial resolution of $28\arcsec$, which is, so far, the largest in M51. There is a correlation between infrared emission (star formation rate indicator) and HCN (1--0) emission (dense gas tracer) at kpc scale in M51, a natural extension of the proportionality between the star formation rate (SFR) and the dense gas mass established globally in galaxies. Within M51, the relation appears to be sub-linear (with a slope of 0.74$\pm$0.16) as $L_{\rm IR}$ rises less quickly than $L_{\rm HCN}$. We attribute this to a difference between center and outer disk such that the central regions have stronger HCN (1--0) emission per unit star formation. The IR-HCN correlation in M51 is further compared with global one from Milky Way to high-z galaxies and bridges the gap between giant molecular clouds (GMCs) and galaxies. Like the centers of nearby galaxies, the $L_{\rm IR}$/$L_{\rm HCN}$ ratio measured in M51 (particularly in the central regions), is slightly lower than what is measured globally in galaxies, yet is still within the scatter. This implies that though the $L_{\rm IR}$/$L_{\rm HCN}$ ratio varies as a function of physical environment in the different positions of M51, IR and HCN indeed show a linear correlation over 10 orders of magnitude. | |
| dc.language.iso | en | |
| dc.publisher | American Astronomical Society | |
| dc.subject.en | Astrophysics - Astrophysics of Galaxies | |
| dc.title.en | Spatially-Resolved Dense Molecular Gas and Star Formation Rate in M51 | |
| dc.type | Article de revue | |
| dc.identifier.doi | 10.1088/0004-637X/810/2/140 | |
| dc.subject.hal | Planète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO] | |
| dc.identifier.arxiv | 1507.08506 | |
| bordeaux.journal | The Astrophysical Journal | |
| bordeaux.page | id. 140 | |
| bordeaux.volume | 810 | |
| bordeaux.issue | 2 | |
| bordeaux.peerReviewed | oui | |
| hal.identifier | hal-01197442 | |
| hal.version | 1 | |
| hal.popular | non | |
| hal.audience | Internationale | |
| hal.origin.link | https://hal.archives-ouvertes.fr//hal-01197442v1 | |
| bordeaux.COinS | ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The%20Astrophysical%20Journal&rft.date=2015-07&rft.volume=810&rft.issue=2&rft.spage=id.%20140&rft.epage=id.%20140&rft.eissn=0004-637X&rft.issn=0004-637X&rft.au=CHEN,%20Hao,&GAO,%20Yu,&BRAINE,%20J.&GU,%20Qiusheng,&rft.genre=article |
Fichier(s) constituant ce document
| Fichiers | Taille | Format | Vue |
|---|---|---|---|
|
Il n'y a pas de fichiers associés à ce document. |
|||