A Local Baseline of the Black Hole Mass - Host Galaxy Scaling Relations for Active Galaxies
The discovery of relations between supermassive black holes (BHs) and their host-galaxy properties has sparked many observational studies pertaining both to the local Universe and cosmic history. Nevertheless, a clear understanding of their origin and fundamental drivers still eludes us. Studying the evolution of these relations depends on our understanding of the slope and scatter of local relations for active galaxies (AGNs). We propose a SNAP program of a unique sample of 84 local type-1 AGNs, spanning a wide range of BH masses (MBH), morphologies, and stellar masses. The high resolution WFC3/F814W images are essential for a detailed decomposition of the host-galaxy in the presence of a bright AGN point source, resulting in precise measurements of the different host-galaxy components and AGN luminosity free of host-galaxy contamination for a robust determination of MBH. When complemented with spatially-resolved Keck spectra to determine stellar-velocity dispersion within bulge effective radius, this yields a most complete baseline of host-galaxy properties over the entire range of MBH scaling relations. A typical SNAP completion rate results in a sample of ~30 objects which will be used to calibrate existing Gemini NIRI and SDSS images. We will study slope and scatter of the relations, dependencies and fundamental drivers. The frequency of pseudo-bulges, bars, and (minor) mergers will reveal the dominant growth mechanism of spheroids. The homogeneous sample will identify any selection biases in the reverberation-mapped AGN sample which serves as a MBH calibrator for the entire Universe. Results will be compared with state-of-the-art semi-analytical models.
This is a SNAP observing proposal of a total of 84 local (z<0.1) type-1 Active Galactic Nuclei (AGNs). We will obtain WFC3/UVIS images in F814W to maximize the contrast between AGN and host, avoiding strong AGN emission lines, while taking full advantage of the high resolution of UVIS. The ETC indicates saturation for the brightest objects (14.8 mag in SDSS i-band) after 20s. To obtain the dynamic range needed for an accurate decomposition of the host galaxy and the AGN, the long exposures will be complemented by short, unsaturated ones. We will take sequences of one short (between 20-100 sec, depending on the object's brightness) and one long exposure (400 sec), one long and one short exposure, to avoid buffer dump (which will occur during the long exposures). POS TARG is used to set up a dither pattern manually that corresponds to the default WFC3-UVIS-GAP-LINE (with center UVIS). The total time including overheads amounts to just under 30 minutes, ideal for a SNAP program. We have split the targets according to their SDSS i-band magnitude in five magnitude bins and used the ETC to calculate the time until saturation and use conservative limits for the short exposures. Full frame read out is necessary to trace the host galaxy disks until the background and to obtain field stars for PSF fitting of the strong AGN point source in the center.
Massive Black Holes And Their Host Galaxies
Galaxies and the IGM
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:pcs-time 333
:si-vis-utilization 1410
:al-overhead-at-end 124
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3449
:pcs-gap 0
)
false
1
0