Bosch 2 608 005 057 Sanding Frame Professional Scientific Communications

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Supplementary observations were gathered from other observatories around the world.

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The mission of the AAS is to enhance and share humanitys scientific understanding of the universe.

It has a worldwide membership of around 50 000 comprising physicists from all sectors, as well as those with an interest in physics.

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Bosch 2 608 005 057 Sanding Frame Professional Scientific Communications

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We have reliably measured the time delay between variations in the continuum and H emission line in six local Seyfert 1 galaxies.

These measurements are used to calculate the mass of the supermassive black hole at the center of each of these AGNs.

We place our results in context to the most current calibration of the broad-line region (BLR) R BLR L relationship, where our results remove outliers and reduce the scatter at the low-luminosity end of this relationship.

We also present velocity-resolved H time-delay measurements for our complete sample, though the clearest velocity-resolved kinematic signatures have already been published.

Examples include correlations between the BH mass and total luminosity of stars in the galactic bulge (the M BH L bulge relationship; Kormendy Richstone 1995; Magorrian et al.

Wandel 2002; Graham 2007; Bentz et al.

BH mass and bulge stellar velocity dispersion (the M BH relationship; Ferrarese Merritt 2000; Gebhardt et al.

Ferrarese et al. 2001; Tremaine et al.

Onken et al. 2004; Nelson et al.

The current thrust to better understand this BHgalaxy connection relies on mass measurements of large samples of BHs in both the local and distant universe.

The masses of BHs in distant galaxies can only be measured indirectly using the scaling relationships mentioned above, as well as the AGN R BLR L relationship (Kaspi et al.

Bentz et al. 2006, 2009b ), which provides the capability to estimate BH masses from a single spectrum of an AGN (Wandel et al.

In order to understand the evolution of BH and galaxy growth over cosmological times, it is useful to compare the location of distant galaxies on these relationships with local samples.

This can only be done by calibrating the local relation with direct BH mass measurements.

Local masses are measured directly in quiescent galaxies using dynamical methods (see Kormendy Richstone 1995; Kormendy Gebhardt 2001; Ferrarese Ford 2005, for reviews) that rely on resolving the motions of gas and stars within the sphere of influence of the central BH and are thus very resolution intensive and only applicable in the nearby universe.

Direct measurements can also be made from observations of megamasers sometimes seen in Type 2 AGNs, but making these observations relies on a particular viewing angle into the nuclear region of these galaxies and is thus not applicable to a large number of objects.

Direct mass measurements can also be made in Type 1 AGNs using reverberation mapping, which is a method that relies on time resolution to trace the light-travel time delay between continuum and broad emission-line flux variations to measure the characteristic size of the broad-line region (BLR).

Using virial arguments, this size is related to the BH mass through the velocity dispersion of the BLR gas, determined from the broad emission-line width.

Although reverberation mapping is technically applicable at all redshifts, the reverberation time delay scales with the AGN luminosity (i.e., the R BLR L relationship), and this coupled with time dilation effects make it difficult and particularly time consuming to make such measurements out to high redshift (see Kaspi et al.

The constraints for making direct BH mass measurements at large distances make the use of the R BLR L relationship particularly attractive for obtaining even indirect mass estimates at all redshifts for which a broad-line AGN spectrum can be obtained.

In addition, masses can be estimated for large samples of objects (e.g., McLure Dunlop 2004; Kollmeier et al.

Salviander et al.

Shen et al. 2008; Vestergaard et al.

BHgalaxy connection and its evolution across cosmic time (e.g., Salviander et al.

Vestergaard Osmer 2009 ).

However, in order to reliably apply these relationships to high-redshift objects and determine any evolution in the relationships themselves, local versions of the relationships need to be well populated with high-quality data, so that calibration of these local relationships is secure (i.e., observational scatter minimized) and any intrinsic scatter is well characterized (see, e.g., Bentz et al.

Graham 2007; Gltekin et al.

Woo et al. 2010, for recent efforts to improve scaling relation calibration and characterization of intrinsic scatter).

Furthermore, systematic uncertainties also need to be understood and minimized so that the local relations, on which all other related studies are based, are as robust as possible.

In this work, we present new reverberation mapping measurements of the BLR radius and BH mass for several nearby Seyfert galaxies from an intensive spectroscopic and photometric monitoring program.

The goals of this program are (1) to improve the calibration of local scaling relationships by populating them with not only additional high-quality measurements, but also replace previous measurements of either poor quality or that were suspect for one reason or another and (2) to take the method of reverberation mapping one step past its currently successful application of measuring BLR radii and BH masses to uncover velocity-resolved structure in the reverberation delays from the H emission line.

Our monitoring program spanned more than four months, over which primary spectroscopic observations were obtained nightly (weather permitting) for the first three months at MDM Observatory.