The Fate of the X-Ray Emitting Gas in the Early-Type Galaxy NGC 5044 X-Ray Brightest Group in the Sky Jeremy Lim William Forman Jan Vrtilek Christine Jones Ewan O’Sullivan Francoise Combes Philippe Salome Simona Giacintucci Alastair Edge Ming Sun O’Sullivan Stephen Hamer Pasquale Temi Henrique Schmitt Youichi Ohyama William Mathews Fabrizio Brighenti Dinh-V Trung

Highly Perturbed X-Ray Morphology Raw 0.5-2.0 keV Chandra ACIS images Many small cavities inflated by repeated AGN outbursts that essentially blow in the wind. Sloshing induced cold fronts. Pcav= 6.5 x 1043 erg s-1 ~ Lx within the central 25 kpc. tcool= 4 x 107 yr Mass deposition rate = 5 M yr-1

Radio Properties of the Central AGN νLν (erg s-1) Many weak AGN outbursts Pcav for smallest X-ray cavity is 3 x 1041 erg s-1 νLν (230GHz) = 500 νLν (630MHz). tage = 5 Myr assuming equipartion and a break frequency of 230 GHz. GMRT data at 235 MHz

CO(2-1) ALMA Observations 24 molecular structures detected above 4σ within the central 2.5 kpc. Mmol = 3 x 105 – 107 M Mmol (tot) = 5 x 107 M σv = 15 – 65 km s-1 Linewidths are too broad to be GMCs and are likely Giant Molecular Associations (GMAs). The GMC filling factor in the few resolved GMAs is 15%.

Comparison of IRAM 30m and ALMA Data at CO(2-1) Good agreement between ALMA and IRAM 30m for redshifted CO emission. The blueshifted IRAM flux is 5 times greater than the blueshifted ALMA flux. This implies that there is a significant amount of large scale (R>300 pc) blueshifted diffuse CO emission that is resolved-out in the ALMA data. IRAM 30m ALMA

High Resolution Spectrum of Most Massive Molecular Structure GMA 18 is well fit with a double Gaussian (σv= 5.5 and 37.5 km s-1). Mmol=1.0 x 107 M rc=140 pc α=5σv2rc/GMmol=24 GMA 18 is not gravitationally bound. GMA 18 is not pressure confined (Pturb > Phot). GMA 18 will dissipate on a timescale t=2rc/σv=10 Myr. The linewidth of the narrow line feature is typical of an individual virialized GMC.

CO(2-1) Position-Velocity Diagram GMAs 13 and 18 are distinct molecular structures No apparent disk-like structures near the central AGN. P-V diagram consistent with infall 

Kinematics of the Molecular Gas GMAs 11 and 13 have velocities near the systemic velocity of NGC 5044 far from the AGN and increasing blueshifted velocities near the AGN. This suggests that these GMAs are falling into the AGN from the far side of the galaxy. The velocity gradient of GMA 18 is perpendicular to that expected for a disk rotating about the AGN.

CO(2-1) Absorption Feature in the AGN Continuum Fitting a Gaussian profile to the absorption feature gives: <v>=260 km s-1 and σv = 5.2 km s-1. For comparison, the circular velocity is 325 km s-1. The linewidth is typical of an individual GMC. Optical depth at line-center is τ=0.35. Either 30% of the 230 GHz emission region is covered by an optically thick cloud or the entire 230 GHz emission region is covered by an optically thin cloud. Assuming the absorption feature is due to a GMC and using a standard linewidth-size relation implies that the 230 GHz emission region is smaller than 50 pc in radius.

Correlations Between the Molecular Gas and Dust and Ha Filaments A few of the GMAs are obviously correlated with dust. A few of GMAs trace the dust filament to the NW. Many GMAs are not associated with dust or Ha emission.

Summary of ALMA Results Source of cold gas: Velocity dispersion of the GMAs is 122 km s-1, which is less than the stellar velocity dispersion of 237 km s-1. Several GMAs are likely on infalling, nearly radial orbits No disk-like structures GMAs have a nearly azimuthially symmetric distribution Mass deposition rate is 25 times greater than the stellar mass loss rate. The molecular gas arises from the thermally unstable hot gas. Supply time is greater than 10 Myr and could be as much as 100 Myr. Dynamics: For buoyancy to be important the AGN inflated cavities much displace a mass equal to the molecular mass. The displaced mass in the X-ray cavities is only 15% of the molecular mass. There are no large scale radio jets in NGC 5044. Molecular structures likely follow ballistic orbits after condensing out of the hot gas. The GMAs are not gravitationally bound or pressure confined and should disperse on a timescale of approximately 10 Myr.

Summary of ALMA Results Star Formation: The observed star formation rate is 0.073 M yr-1 (Werner et al. 2014). Based on the Kennicutt-Schmidt relation, the total star formation rate from the three best resolved GMAs is 0.03 M yr-1 . Since these three GMAs comprise 35% of the total molecular mass, there is reasonable good agreement with the observed star formation rate. The depletion time of the molecular gas due to star formation is 700 Myr. Assuming one SNeII for each 100 M of gas consumed into stars, implies that SNeII will produce an energy equivalent to 60% of the total turbulent kinetic energy in GMA 18 over its lifetime.