2011A&A...528A..30C


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.21CET11:08:14

2011A&A...528A..30C - Astronomy and Astrophysics, volume 528A, 30-30 (2011/4-1)

Molecules as tracers of galaxy evolution: an EMIR survey. I. Presentation of the data and first results.

COSTAGLIOLA F., AALTO S., RODRIGUEZ M.I., MULLER S., SPOON H.W.W., MARTIN S., PEREZ-TORRES M.A., ALBERDI A., LINDBERG J.E., BATEJAT F., JUETTE E., VAN DER WERF P. and LAHUIS F.

Abstract (from CDS):

We investigate the molecular gas properties of a sample of 23 galaxies in order to find and test chemical signatures of galaxy evolution and to compare them to IR evolutionary tracers. Observation at 3mm wavelengths were obtained with the EMIR broadband receiver, mounted on the IRAM 30m telescope on Pico Veleta, Spain. We compare the emission of the main molecular species with existing models of chemical evolution by means of line intensity ratios diagrams and principal component analysis. We detect molecular emission in 19 galaxies in two 8GHz-wide bands centred at 88 and 112GHz. The main detected molecules are CO, 13CO, HCN, HNC, HCO+, CN, and C2H. We also detect HC3N J=10-9 in the galaxies IRAS 17208, IC 860, NGC 4418, NGC 7771, and NGC 1068. The only HC3N detections are in objects with HCO+/HCN<1. Galaxies with the highest HC3N/HCN ratios have warm IRAS colours (60/100µm>0.8). The brightest HC3N emission is found in IC 860, where we also detect the molecule in its vibrationally excited state. We find low HNC/HCN line ratios (<0.5), that cannot be explained by existing PDR or XDR chemical models. The intensities of HCO+ and HNC appear anti-correlated. No correlation is found between the HNC/HCN line ratio and dust temperature. All HNC-bright objects are either luminous IR galaxies (LIRG) or Seyferts. Galaxies with bright polycyclic aromatic hydrocarbons (PAH) emission show low HNC/HCO+ ratios. The CO/13CO ratio is positively correlated with the dust temperature and is generally higher than in our galaxy. The emission of CN and C18O is correlated. Bright HC3N emission in HCO+-faint objects may imply that these are not dominated by X-ray chemistry. Thus the HCN/HCO+ line ratio is not, by itself, a reliable tracer of XDRs. Bright HC3N and faint HCO+ could be signatures of embedded star-formation, instead of AGN activity. Mechanical heating caused by supernova explosions may be responsible for the low HNC/HCN and high HCO+/HCN ratios in some starbursts. We cannot exclude, however, that the discussed trends are largely caused by optical depth effects or excitation. Chemical models alone cannot explain all properties of the observed molecular emission. Better constraints to the gas spacial distribution and excitation are needed to distinguish abundance and excitation effects.

Abstract Copyright:

Journal keyword(s): evolution - ISM: molecules - galaxies: evolution - galaxies: ISM - galaxies: active

Simbad objects: 30

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Number of rows : 30

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 2865 2
2 NGC 660 LIN 01 43 02.350 +13 38 44.45   12.02 11.16     ~ 501 2
3 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 3993 2
4 NGC 1056 Sy2 02 42 48.287 +28 34 27.36   13.5       ~ 139 0
5 NGC 1140 EmG 02 54 33.5258827369 -10 01 43.135585379 12.41 12.84 12.49 13.6 13.5 ~ 254 1
6 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 373 3
7 NGC 1377 GiG 03 36 39.077 -20 54 08.14   13.38   12.12   ~ 181 0
8 IC 342 SBG 03 46 48.514 +68 05 45.98   10.5       ~ 1364 1
9 UGC 2866 GiG 03 50 15.0017250839 +70 05 40.331792502   15.5       ~ 63 1
10 NGC 1614 AGN 04 34 00.027 -08 34 44.57   14.66 13.99     ~ 594 0
11 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 812 1
12 NGC 2273 Sy2 06 50 08.6724567505 +60 50 44.879789544   14.50 13.54     ~ 445 3
13 UGC 5101 Sy1 09 35 51.694 +61 21 10.52   15.20 15.50     ~ 500 4
14 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5226 6
15 NGC 3079 Sy2 10 01 57.80342 +55 40 47.2428 11.57 11.54 10.86     ~ 1220 3
16 M 108 SBG 11 11 30.967 +55 40 26.84   10.70       ~ 402 1
17 NGC 4194 AGN 12 14 09.615 +54 31 35.93   13.79 13.30     ~ 403 2
18 NGC 4388 Sy2 12 25 46.820 +12 39 43.45 11.91 11.76 11.02     ~ 1155 2
19 NGC 4355 Sy2 12 26 54.628 -00 52 39.51   14.21 13.37     ~ 388 2
20 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1739 3
21 IC 860 LIN 13 15 03.51 +24 37 07.8   14.8       ~ 172 0
22 2MASX J15265942+3558372 LIN 15 26 59.425 +35 58 37.23   15.61       ~ 243 1
23 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2628 4
24 NGC 6090 PaG 16 11 40.3 +52 27 21   14.0       ~ 392 2
25 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1447 2
26 6dFGS gJ172322.0-001701 LIN 17 23 21.943 -00 17 00.96   15.1       ~ 368 0
27 NGC 7023 BNe 21 01 36.9 +68 09 48   7.20       ~ 604 0
28 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1845 3
29 NGC 7674 Sy2 23 27 56.6974755223 +08 46 44.238278540 13.84 13.92 13.23 12.64   ~ 621 4
30 NGC 7771 GiG 23 51 24.880 +20 06 42.57 13.42 13.08 12.25     ~ 307 4

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2019.11.21-11:08:14

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