Results from ifa, HawaiiResults from ifa, Hawaii

On behalf of Treister, Kartaltepe, CowieTomo Goto

Ifa FMOS programs

● Treister etal. 10B, 11A● Kartaltepe, Sanders etal. 10B● Cowie etal. 10B, 11A

Treister et al. 10B,11AThe main goal of this program is to identify and measure redshifts for heavily-obscured AGN candidates selected in the mid-IR. Most of these sources are expected at 1<z<3.We observed with FMOS on Nov 20 two fields for ~5 hours each on (~3 hours of effective exposure time), CDFS and COSMOS. Then on Feb. 12,13 on CDFS,COSMOS and BOOTES.

CDFS

COSMOS

One of the examples of these sources, a clear AGN (based on the emission lines) at z=1.25,

Kartaltepe, Sanders et al.(COSMOS, 24um, 70um sources)

We targeted a combination of IR selected galaxies (both 70 and 24 micron selected) and AGN (many of which are also in the IR category) in the photz ranges where we would expect to see emission lines.

Overall, I was very happy with the run and the performance. So far, it looks like the depth we reached is pretty close to what was expected based on the sensitivities on the website. I am very encouraged by the initial results. The instrument behaved alright. There were usually a few fibers that got stuck during the allocation process but I suppose out of 200 fibers this isn't such a huge loss. The fiber allocation software is ok, but still a little buggy. For now, it is very difficult to allocate single fibers after automatically allocating the fiber pairs. It is almost too automated in a way, I would like to be able to select, de-select fibers on the fly. The reduction pipeline software also seems to be working pretty well so far, no major problems there yet :)

●24um selected AGN at z~1.5.

Cowie et al.

a) previously unidentified quasar in the GOODS-S/CDFS 4Ms region.b) previously unidentified strong emission-line galaxy in the GOODS-S regionc) known redshift galaxy in the GOODS-S where we were trying to measure the strength of the H alpha line and the NII/H alpha ratio to estimate metallicity.

Comparison with G140L on HST

I have also attached some comparison spectra from theG140L grism on HST. These are in the GOODS-N. The grism spectra are quite sensitive but the low resolutionmeans H alpha and NII are totally blended and eventhe OIII doublet is a a blend. One interesting possibilityis to take a sample of emitters selected with HST andthen use FMOS to get the higher resolution observations.We are going to try this in our March FMOS run.

Summary● Overall, ifa is happy with the FMOS

performance & data.● Minor problems with fiber allocation software.● Grateful to intense support on observation,

data reduction...etc by the FMOS team and Subaru staff.

● “This is the first time, I got reduced data delivered by the end of the night!” (E.Treister)

● Special thanks to Tamura-san, Aoki-san, Yabe-san, Iwamuro-san,,,and many others in the FMOS team and Subaru staff.