VIMOS Science Verification Programs at Melipal/UT3
Programs selected for VIMOS Science Verification
- A VIMOS-IFU Study of Early-Type Galaxies
- Globular Clusters of NGC5128
- A Deep IFU Study of A1689
- The galaxy cluster RXCJ1131.9-1955 at z=0.3
- VIMOS Home Page
- VIMOS Exposure Time Calculator: [imaging ] [MOS] [IFU]
- VLT Science Verification Policy and Procedures
- VIMOS SV Team
Objective: The panoramic integral-field mode of VIMOS offers the unique capability of spectroscopically mapping the complete two-dimensional kinematics of stars and gas in nearby early-type galaxies. The science goals are to determine the dynamical structure of the galaxies, to connect the internal dynamics to the age and metallicity of the stars, and to establish the metal enrichment and assembly history of these systems.
NGC 1427 (03h42m19.4s -35d23m34s)
NGC 3379 (10h47m49.6s +12d34m55s)
NGC 3384 (10h48m17.0s +12d37m47s)
NGC 4365 (12h24m28.2s +07d19m03s)
IFU, HR-blue grating (approx. 4100 - 6100 A, 0.51 A/pix)
NGC 1427: 1 central IFU pointing, 3x1800s exposures
NGC 3379: 1 central IFU pointing, 3x1800s exposures
NGC 3384: 1 central IFU pointing, 3x1800s exposures
NGC 4365: 1 central IFU pointing, 3x1800s exposures
clear/thin clouds, seeing 0.8-2.0arcsec
Objective: We will obtain spectroscopy of globular clusters in NGC 5128 out to radii of 20 arcmin (or ~5 effective radii) to provide absorption-line indices and globular cluster mean velocities. The absorption-line indices can be used to constrain ages and metallicities of the stellar populations of globular clusters. The velocities can be used to infer the galaxy gravitational potential (i.e., oblate/prolate, triaxial).
NGC 5128 (13h25m27.6s -43d01m09s)
MOS, HR-blue grating
4 hours x 4 pointings = 16 hours
- Conditions:Pre-imaging obtained at ~0.6''-1.0'' seeing. MOS observations to be performed.
G. Verdoes Kleijn
Objective: We plan to obtain 3D spectroscopy of highly magnified regions of the cluster Abell 1689. Four VIMOS IFU pointings will target the critical curve of the cluster (lines of infinite magnification). The wavelength coverage from 5500A to about 9000A will allow to search for star-forming galaxies in the redshift range 3.5<z<6 through their Lya alpha emission. Literature work shows (e.g. Ellis et al 2001) that even with longslit spectroscopy this approach is efficient in locating intrinsically faint but highly magnified star-forming galaxies, presumably the first forming objects (galaxy building blocks). The use of the VIMOS IFU will highly enhance the search efficiency.
A1689 (13:11:34.2, -01:21:56.0)
IFU, Intermediate resolution spectroscopy
5 hours per pointing
Program to be observed
Objective: RXCJ1131.9-1955 is one of the most X-ray luminous galaxy clusters in the ROSAT All-Sky Survey at a redshift of z = 0.3 and also one of the most massive clusters as revealed by follow-up XMM Newton observations. With VIMOS spectroscopy we can obtain for the first time a very comprehensive account of the galaxy population mix and star formation rate of the galaxy population of the cluster and get a detailed picture of the cluster dynamics. Choosing a very massive cluster as a target we are making optimal use of the VIMOS multiplex capabilities collecting cluster galaxy spectra for at least 1/3 to 1/2 of the galaxies visibile down to 23mag in R.
RXCJ1131.9-1955 (11 31 40.8, -19 54 00 / 11 32 20.4, -19 51 48)
2 hours per pointing (low-resolution), 3 hours per pointing (medium-resolution)
Program to be observed.