A dataset provided by the European Space Agency

Name OT2_kdasyra_2
Title The role of AGN feedback in increasing the turbulence of the molecular gas: lessons from the warm phase
URL

http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342241845&instrument_name=PACS&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342241845&instrument_name=SPIRE&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342241846&instrument_name=PACS&product_level=LEVEL0&compress=true
http://archives.esac.esa.int/hsa/whsa-tap-server/data?retrieval_type=OBSERVATION&observation_id=1342241846&instrument_name=SPIRE&product_level=LEVEL0&compress=true

DOI 10.5270/esa-ldgrxxt
Author dasyra, k.
Description Feedback mechanisms, i.e., jets, winds, and radiation pressure from active galactic nuclei (AGN) are thought capable of suppressing or triggering star formation in their host galaxies. Their past occurrence might have even affected the observed luminosity functions of present-day galaxies. AGN feedback signatures have been mainly sought for in OH, OH+, H2O, and H20+ absorption line profiles with Herschel. Similar queries with the high-J CO emission lines have not been performed even though they are feasible. We propose to look for feedback effects in high-J CO lines in 6 local AGN that are unique for this purpose. They have highly turbulent motions of warm H2 gas, as seen with Spitzer (Dasyra & Combes 2011). Their H2 lines are both very broad and strong, with typical velocity dispersions of 200-300km-s and M_H2-LIR ratios 5-160 times higher than that of Mrk231. In 4C12.50, the H2 line wings indicate the presence of a massive (5*10^7M_sun) outflow. If the strong H2 emission originates from gas shocked by AGN feedback mechanisms, it can be associated with strong high-J CO emission. Our sources allow for a direct comparison not done before: that of the gas velocity dispersion as probed by the two most abundant molecules, H2 and CO, in the T range where this becomes possible. We will also: (i) compare the widths of high and low J CO lines, (ii) locate the emission peak of the warm gas, (iii) model its excitation mechanism, and (iv) query for outflow-related line wings. Upon success, we will compute the warm gas mass (fraction) that the outflow entrains. The flow rate will be compared with the star-formation rate to indicate if the outflow is AGN driven, and if it can quench star formation. To achieve our goals we propose to observe with PACS the CO (15-14) and (18-17) lines in all 6 AGN, complementing them with PACS data of the [CII], [OI] 63 and 146 micron lines, and SPIRE spectra, when not available. The time investmen...
Publication
Instrument PACS_PacsRangeSpec_point
Temporal Coverage 2012-03-18T21:51:45Z/2012-03-18T22:21:05Z
Version SPG v14.2.0
Mission Description Herschel was launched on 14 May 2009! It is the fourth 'cornerstone' mission in the ESA science programme. With a 3.5 m Cassegrain telescope it is the largest space telescope ever launched. It is performing photometry and spectroscopy in approximately the 55-671 ┬Ám range, bridging the gap between earlier infrared space missions and groundbased facilities.
Creator Contact https://support.cosmos.esa.int/herschel/
Date Published 2012-09-18T22:06:42Z
Publisher And Registrant European Space Agency
Credit Guidelines European Space Agency, 2012-09-18T22:06:42Z, OT2_kdasyra_2, SPG v14.2.0. https://doi.org/10.5270/esa-ldgrxxt