The MAGPOP-ITP dwarfs sample

1. The MAGPOP-ITP dwarfs sample A. Gil de Paz (UCM), C. Carretero (IAC), I. Pérez-Martín (Groningen), A. Boselli (LAM), J. Gorgas (UCM), R. Peletier (Groningen) & the MAGPOP-ITP collaboration

2. Sample Selection • VIRGO: Starting from the VCC catalogue of Binggeli et al. (1985) we imposed: • B<15 (Mr<-15) in order to ensure that the objects would be detectable with the instrumentation configurations proposed. • Covered by one of the GALEX deep imaging surveys (DIS,NGS,MIS) or the GALEX dedicated imaging survey of Virgo. • The final number of targets: ~90 • FIELD: Starting from the SDSS DR4 we imposed the following selection criteria: • 0.00125 < z < 0.00625 (5-25 Mpc) • -18 < Mr < -15. The bright limit ensures that we are dealing with truly dwarfs- The faint limit guarantees that we are selecting the same population of galaxies both in the field and in Virgo. • -10 dg < Dec < 75 dg and 1h < RA < 11h or 13h < RA < 17h. These limits are imposed by the visibility of the targets and the exclusion of the Virgo area. • As in the case of the Virgo sample we selected only those that had been covered by one of the GALEX deep imaging surveys at least in one of its bands. • The final number of targets: 34

3. Star-forming / Quiescent • VIRGO SAMPLE: Based on the visual morphological classification by Binggeli et al. (1985). u-g=1.2 u-g=1.2

4. Star-forming / Quiescent • FIELD SAMPLE: Using FUV-NUV=0.9 or u-g=1.2 for those objects not detected in the FUV (both the Virgo and Field samples are primordially optically selected): Virgo Q Virgo Q u-g=1.2 FUV-NUV=0.9 Virgo SF Field Virgo SF Field

5. FIELD SAMPLE:

6. FIELD SAMPLE: SDSS (Dolf Michielsen) and GALEX (AGdP) surface photometry already done. See Alessandro’s talk for the status on the ITP observations. ID0615 GALEX ID0615 SDSS-r ID0118 GALEX ID0957 GALEX