SpringerLink
ForumSpringerAstron. Astrophys.
ForumWhats NewSearchOrders


Astron. Astrophys. 325, 769-781


Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

Molecular gas in the barred spiral M 100

I. The IRAM 30m map

M.J. Sempere and S. García-Burillo

Observatorio Astronómico Nacional, Campus Universitario, Apartado 1143, E-28800 Alcalá de Henares (Madrid), Spain
(sempere@oan.es, burillo@oan.es)

Received 30 January 1997 / Accepted 10 March 1997

Abstract

We present a study on the distribution, kinematics and evolution of the molecular gas disk in the barred SBbc spiral M100(NGC4321). The J=2-1 and J=1-0 lines of 12CO have been mapped with the IRAM 30m telescope, with resolutions HPBW=12FORMULA and HPBW=21FORMULA , within the inner 8kpc of the disk (1FORMULA =82pc, assuming DM100=17.1Mpc). Complementary 13CO(1-0) observations of the nucleus, spiral and interarm regions are used to study the nature of H2 gas.

CO emission traces a markedly asymmetric two spiral-arm structure stretching out from a molecular gas bar. The CO bar has a diameter D ~ 90FORMULA and it is aligned with the stellar bar seen in I and K band images (PA=110FORMULA ). Arm I (II) springs off the western (eastern) side of the bar at r ~ 50FORMULA . Arm II is split up in two armlets (at r ~ 40-50FORMULA ), it disappears and finally shows up at a position angle close to the major axis northern crossing (PA=330FORMULA ). The splitting starts near the inner 3::1 resonance identified by Elmegreen et al (1992) in the enhanced optical images of M100. Molecular gas in the bar is strongly concentrated in a nuclear disk of r FORMULA 30FORMULA and M(H2)nucl=2.8 109M FORMULA .

Arms I-II display different arm-interarm contrasts (on average, Ra/ia(CO) increases with radius from 2.5 (r ~ 30FORMULA ) up to 6.5 (r ~ 110FORMULA ), being higher for arm I than for arm II. Also arms I-II relate differently to other spiral arm tracers, underlying the asymmetry in the disk. Comparison between CO, H I and H FORMULA maps show that there is no coherent sequence in the relative location of the star formation tracers along the spiral arms. Evidences of triggering of star formation along spiral arms are poor: Ra/ia(H FORMULA ) is only ~ 2 R(CO) and systematic offsets between H FORMULA and CO ridges (expected to lie downstream and upstream the spiral potential minimum, respectively, assuming trailing arms inside corotation) are hard to find and at places they are absent or even inverted.

CO reveals as the best tracer of gas kinematics in the inner disk. The CO rotation curve (Vrot) is steeper than the curves derived from the H I and H FORMULA data. Vrot reaches 200km s-1 in less than 1kpc. The signature of the m=3 instability has been also identified in the CO derived velocity field. The magnitude and the sign of streaming motions, associated with the spiral arms and the bar, are consistent with the CO disk to be inside corotation (rcor=110FORMULA ). A secondary wave compression develops in the eastern side where arm II is split.

Massive star formation (MSF) is inhibited along the gaseous bar, indicating that M100 is an evolved barred system (Friedli and Benz, 1995). Star formation rate (measured as the ratio SFR=F(H FORMULA )/ICO) is lower for the nuclear disk than for the disk itself. However we suspect the measurement of SFR to be subjected to major uncertainties: the X=N(H2)/ICO conversion factor might be 3 times lower than implicitly assumed and to vary within the disk (lower for the interarm than for the arms and nuclear region) . Moreover extinction affects F(H FORMULA ) mostly in the nucleus where the classical Schmidt law breaks down paradoxically (SFR FORMULA N FORMULA , FORMULA 1). MSF is set on at a distance r FORMULA 12kpc where N(H2) approaches the Toomre (1964) gravitational instability threshold (N FORMULA 7M FORMULA ). Also for r<rc, the neutral gas is mostly in the H2 phase. H I is underabundant in the inner 6kpc and cannot be accounted for by photodissociation of H2 by H II regions.

Asymmetry in the observed molecular gas distribution and kinematics of M 100 seems related with the three-arm structure studied by Elmegreen and collaborators. Although the m=2 spiral mode is still predominant in M100, other secondary modes seem at interplay reflecting the secular evolution of the disk. Compared to M51, M100 appears as an evolved barred spiral.

Key words: galaxies: kinematics and dynamics of - galaxies: spiral - galaxies: individual - radio lines

Send offprint requests to: S. García-Burillo


© European Southern Observatory (ESO) 1997

Online publication: September 9, 1997
Last change: April 28, 1998
helpdesk.link@springer.de