Direct Detection and Mapping of Star Forming Regions in Nearby, Luminous Quasars
We propose to carry out narrow-band emission line imaging observations of 8 quasars at z=0.05-0.15 with the WFPC2 ramp filters and with the NICMOS narrow-band filters. We will obtain images in the [O II], [O III], H-beta, and Pa-alpha emission line bands to carry out a series of diagnostic tests aimed at detecting and mapping out star-forming regions in the quasar host galaxies. This direct detection of star-forming regions will confirm indirect indications for star formation in quasar host galaxies. It will provide a crucial test for models of quasar and galaxy evolution, that predict the co-existence of starbursts and "monsters" and will solve the puzzle of why different indicators of star formation give contradictory results. A secondary science goal is to assess suggested correlations between quasar luminosity and the size of the narrow-line region.
Our targets consist of 8 PG quasars drawn from the Spitzer IRS sample of Schweitzer et al. (2006). We selected all the objects at z<0.15 whose redshifts are such that their Pa-alpha lines fall within one of the available NICMOS narrow-band filters. They have absolute V magnitudes between -22 to -24 and 2-10 keV X-ray luminosities of order 10^43-10^44 erg/s. At the distances of these objects 0.1 arcsec corresponds to 90-260 pc.
We propose to obtain narrow-band images in the [OII]3727, H-beta, [OIII]5007 lines, using the WFPC2 ramp filters (width=1%). In three cases we will be able to obtain [OII] images through the conventional narrow-band filters. The location of the target on the WFPC2 chips is set by the desired wavelength, therefore, we will mostly be using the WF chips (the resolution of our line-ratio maps, will be limited by the images with the lowest resolution). We will carry out sub-pixel dithering to improve the resolution as much as possible. We will also obtain Pa-alpha narrow-band images using NIC2 and NIC3 and the available filters (widh=1%). The angular resolution element and angular pixel size of the NIC3 images will, unfortunately, be rather large and they will limit the resolution of the extinction maps produced via the Pa-alpha/H-beta ratio. The field of view of the WFPC2 ramp filters is ~10 arcsec, which is adequate for our purposes.
In addition to the on-band observations, we will also obtain off-band observations (for continuum subtraction) with medium-band filters and short observations of a PSF star with the same ramp filters and at the same detectors position as the quasars. An image in the WFPC2 F467M filter is suitable for continuum subtraction for all the optical emission-line images because this filter covers a band between the [O II] and H-beta lines. The only emission line of note within its passband is H-gamma, but its flux will be diluted so that it becomes negligible. Bennert et al. (2002) have shown that medium-band filters produce continuum images that are suitable for continuum subtraction (just as good as narrow-band images). The PSF star observations will be used for a careful subtraction of the unresolved quasar emission from the image. This is important for our goal of detecting star-forming regions very close to the active nucleus (a linear distance of 0.3 kpc, corresponding to 0.2-0.3 arcsec). Some of Our proposed targets were also imaged with WFPC2, ACS, and NICMOS with broad-band filters, namely WFPC2 F814W and ACS F550M or F625W). Thus we will be able to use those images of the host galaxies to verify and refine our background subtraction procedures (following Bennert et al. 2002).
To estimate the required exposure times, we used the FIR (8-1000 micron) luminosities listed in Table 1 to compute the H-beta fluxes. These two quantities are related to the star-formation rate [equations (2) and (4) of Kennicutt (1998)] and are therefore connected to each other via L(H-beta)=0.017 L(FIR). Furthermore, we assumed (conservatively) that [OII]/[OIII]=[OIII]/H-beta=1 in order to estimate the [OII] and [OIII] fluxes. The Pa-alpha fluxes were estimated assuming that Pa-alpha/H-beta=0.47 (Osterbrock 1989). Adopting these emission line fluxes and assuming that the emission-line regions are approximately 3 arcsec (~3 kpc) across, we used the WFPC2 exposure time calculator to compute the exposure time needed to reach a S/N~10 per resolution element. This is the minimum S/N needed to distinguish between different excitation mechanisms in the BPT (line-ratio) diagrams at approximately the 3-sigma level. Our estimates are conservative because the star-forming regions are likely to have bright knots that are more easily detectable.
We find that in order to meet the above requirements, we need 2-4 orbits per object for the [OII] images, 1-2 orbits per object for each of the [OIII] and H-beta images, and 1 orbit per object for the Pa-alpha images. For two quasars (PG 0026+129 and PG 1307+085) we will use archival [OIII] images (Bennert et al. 2002). Included in our orbit estimates is the time for on-band images in the emission-line filters and off-band images in medium filters (WFPC2 F467M, NIC2 F237M, and NIC3 F222M). The visibility periods of our targets range from 51 to 57 minutes, leaving approximately 31-36 minutes of exposure time per orbit. Thus, we expect to achieve S/N~10-16 per 0.1 arcsec bin in an integer number of orbits per object.
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J2000
00 29 13.6900
+13 16 3.90
J2000
GALAXY
QUASAR
STAR FORMING REGION
STARBURST
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
08 44 45.6300
+76 53 9.40
J2000
GALAXY
QUASAR
STARBURST
STAR FORMING REGION
This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
12 46 35.2900
+02 22 8.30
J2000
GALAXY
QUASAR
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This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
13 09 47.0300
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J2000
GALAXY
QUASAR
STARBURST
STAR FORMING REGION
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
14 51 8.7800
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J2000
GALAXY
QUASAR
STAR FORMING REGION
STARBURST
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
16 13 57.2000
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J2000
GALAXY
QUASAR
STARBURST
STAR FORMING REGION
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
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J2000
GALAXY
QUASAR
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This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
22 17 12.2600
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J2000
STAR
K V-IV
This object was generated by the targetselector and retrieved from the GSC 2.3 database.
B=12.51+/-0.23; K=8.65
GS60200264
NB70000216
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