SDSS-RM is the first RM campaign to systematically explore the potential of RM at z>0.3, and for all major broad lines (Hbeta, Halpha, MgII, CIII], CIV, etc.) covered in the SDSS spectral range. Other than the limiting magnitude, the sample is an unbiased selection in quasar parameter space. It is designed as a pathfinder for future, large-scale multi-object RM campaigns, but still has the promise to deliver a large sample of quasars with RM detected time lags between the broad line emission and the continuum. Such a sample will substantially improve our understandings of the broad line region structure and calibrations of the BLR radius-luminosity relation, as well as provide reliable estimates of quasar BH masses up to high redshift. In addition to RM science, the photometric and spectroscopic data sets will enable a broad range of important science, including quasar variability, deep spectroscopy of quasar absorption lines, quasar host properties, correlations between BH mass (from RM) and host properties, etc., and will have legacy value and promote multi-wavelength synergy for the years to follow.
Our RM field is one of the PanSTARRS Medium Deep fields, with high-cadence (4-day) multi-band PS1 light curves for all of our targets in 2011-2013. Therefore expanding our baseline 6-month program into the SDSS-IV regime will take full advantage of these PS1 earlier light curves, and detect RM lags on longer timescales (>6 months in the observed frame). Such an extended program will fully cover the parameter space of redshift versus time lags for a large, homogeneous quasar sample.
PIs: Yue Shen (Carnegie) and Niel Brandt (Penn State)
CFHT imaging PI: Patrick Hall (York)
To retrieve raw or ELIXIR-reduced CFHT+MegaCam images, go to the CADC Advanced Search Page and under Observation Constraints, click on P.I. Name, and search on "Patrick Hall". Other constraints can also be applied.
The ELIXIR metadata FITS file and other information can be obtained from this page at CFHT.
MegaCam observations are use both g and i filters. In each filter, two images are taken at each pointing, with one exposure time shorter than the other to extend the dynamic range of the photometry. Summed exposure times per dither per epoch are nominally 78 seconds in g and 111 seconds in i. Most sky positions will be covered by two dithers. To cover the 3-degree-diameter spectroscopic field, we use nine overlapping MegaCam pointings (A through I), each with two dithers (1 and 2). The RA and DEC values for positions A1 through I2 are given in the table below.
|
Position |
RA |
DEC |
|
A1 |
14:14:47.17 |
+53:05:46.0 |
|
A2 |
14:14:50.83 |
+53:03:31.0 |
|
B1 |
14:14:47.19 |
+52:07:00.5 |
|
B2 |
14:14:50.81 |
+52:04:45.5 |
|
C1 |
14:08:43.77 |
+52:09:50.0 |
|
C2 |
14:08:47.54 |
+52:07:35.0 |
|
D1 |
14:08:15.56 |
+53:05:46.0 |
|
D2 |
14:08:19.40 |
+53:03:31.0 |
|
E1 |
14:08:35.77 |
+54:01:42.0 |
|
E2 |
14:08:39.63 |
+53:59:27.0 |
|
F1 |
14:14:47.15 |
+54:04:31.5 |
|
F2 |
14:14:50.85 |
+54:02:16.5 |
|
G1 |
14:20:58.53 |
+54:01:42.0 |
|
G2 |
14:21:02.07 |
+53:59:27.0 |
|
H1 |
14:21:18.77 |
+53:05:46.0 |
|
H2 |
14:21:22.26 |
+53:03:31.0 |
|
I1 |
14:20:50.61 |
+52:09:50.0 |
|
I2 |
14:20:54.08 |
+52:07:35.0 |