Connection between Super massive black holes and star formation rate in CALIFA galaxies


SMBH-SFRconnectionwithCALIFAgalaxies We investigated the connection between the growth of the central black hole and the star formation rate of galaxies with integral field spectroscopy (IFS) observations available with the sample of the Calar Alto Legacy Integral Field Area Survey (CALIFA) survey. For this, we selected 85 AGN\(+\)TO galaxies obtained from the DR3 of CALIFA. These galaxies were selected because they have previous estimations of disk-bulge decomposition available. The IFS were processed with synthesis population techniques using the STARLIGHT (citation not found: starlight) code, from which we were able to get the stellar velocity dispersion of the galaxy bulges and calculate the mass of the central black hole through the bulge mass - black hole mass relation (citation not found: mcconnell13). Furthermore, the synthesis population technique lets us to get the mean age of the stellar populations. The star formation rates were obtained from the H\(\alpha\) emission lines. We compared the mass of the central black hole (M\({}_{\bullet}\)) with the star formation rates in pixels out of the bulge. We found that the star formation decreases when the range of M\({}_{\bullet}\) increases. We think it is not a direct but circumstantial connection.



The data consists in 85 data cubes available from the CALIFA-DR3 survey (citation not found: califa2016). The data cubes correspond to AGN+TO galaxies (according to the BPT diagram based in the SDSS spectral, (citation not found: abazajian2009)) which also have bulge-to-disk descomposition available taken from (citation not found: mendez2016). The descomposition of (citation not found: mendez2016) offers the effective radius (R\({}_{e}\)) of the bulge for g, r, and i band. The data cubes normally consists in arrays of 78\(\times\)77 spaxels with an individual size of 1’’ each one. Each spaxel contains an spectrum that cover a wavelength depending on one of the two gratings used by the CALIFA survey: V500 at a resolution of 6.0 Å FWHM which cover a range from 3700 to 7500 Å and V1200 at a higher resolution of 2.3 Å FWHM, but with a lower range from 3700 to 4200 Å. In most cases the data cubes of V500 and V1200 were combined to form the COMB data cubes, which have a similar wavelength range that V500 but the flux was averaged in the overlaped region between the setups. To do that the resolution of V1200 was degraded and centered to the V500. In this work we used the COMB data cube when it was available. Otherwise the V500 cube was used. Tabla (xxx) contains the main information of the galaxies, including the setup, mass and kind of activity.