the local universe survey (lus)
Post on 06-Feb-2016
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The Local Universe Survey (LUS)IAA IAC INAOE UAM
J.M. Vilchez J.M. Rodríguez Espinosa
R. Terlevich A. I. Díaz
Jorge Iglesias C. Muñoz Tuñón D. Rosa M. Mollá (Ciemat)
A. López Aguerri O. Vega
J. Mendez Abreu D. Mayya
L. Rodríguez
E. Terlevich
E. Bertone
A. Bressan
LUS
• LUS aims to study the formation and evolution of galaxies– Determine the spatial distribution of the properties of
the ionised gas and recent star formation– Determine the spatial distribution of the properties of
the evolved stellar populations• Local Universe Galaxies carry themselves the
memory of its formation and evolution (e.g. Heavens et al., Nature 2004; R. González Delgado, this morning talk!)
LUS: The Goals• Trace the star formation history of individual galaxies
in the sample• Produce high-resolution BPT-diagram analysis• Map the metallicity/age distribution in disc galaxies• Study Compact Star Clusters in the nuclear and
circumnuclear regions of normal galaxies• Study Feedback: the interaction between massive
stars and the ISM• Detect and quantify the diffuse ionized gas in the
sample galaxies• Study Star-formation in low-density environments
The Sample
• All galaxies inside a volume of 3.5 Mpc• Plus all irregulars and spirals within a volume of 11
Mpc• Plus a sample of Virgo Galaxies
• 224 Galaxies in Total
LUS strategy• Map the sample galaxies in both a number of selected
emission lines plus continuum• The lines selected are Lick indices motivated• Use Galex, SDSS, 2Mass & Spitzer BB photometry• The logistics is dictated by the need to cover most
relevant lines and continuum feature sparing observing time
• Use the OSIRIS TF and BB for the observation• Preliminary results show that to achieve our goals we
require narrow band images with photometric accuracy < 5% ...
What we have so far6 hours Verification Time 6 hours on Spain-Mex. 9 hours Spain-Mex.
M101 Field SE M101 Field SW NGC 5949BB: u,i BB: u,i BB: u, g, r, i
TF: Hα + [NII] (6528,6548,6568,6588,6608,6628,6648,6668)
TF: Hα + [NII] (6528,6548,6568,6588,6608,6628,6648,6668)
TF: Hα (6572, 6533)TF: [NII] (6593, 6617)
TF: [SII] (6696,6716,6736,6756,6776,6796,6816)
TF: [SII] (6696,6716,6736,6756,6776,6796,6816)
TF: [SII] (6726, 6702)[SII] (6740, 6716) (planned)
TF:[ SIII] (9056,9076,9096,9116,9136,9156,9176)
TF:[ SIII] (9056,9076,9096,9116,9136,9156,9176)
TF: [SIII] (9082, 9110) (planned)
M101
M101 region Hα
M101 region SII
The LUS Pipeline (IRAF based)• Pre-reduction: bias, flat, and trim• Each chip treated individually• Cosmic Ray and Bad Pixel Masking (pending)• Alignment of the images: geomap, geotran and
imcombine• Create a Weight image by combining 1 – 0 fake images
using the same dithering pattern as for the real images• PSF-Matching before stacking (pending)• Astrometry and creation of a single image: ccxymatch,
ccmap, imcombine, mkpattern, ccsetwcs, wregister (applied to the images and the weight)
Example: NGC 5949
LUS Pipeline: Step II• Flux calibrate using the S3 Method:• Select isolated SLOAN stars• Use the SEGUE spectroscopic data base to
fit the observed SEDs (http://segue.uchicago.edu/)
• Use best Spectra to find the conversion between counts and flux in the NB TF images
NGC 5949
SLOAN Id K factorHα Image (λc=6572 Å, Δλ=12 Å)
J152726.30+644617.1 1.67239e-17J152731.33+644205.4 1.34703e-17J152737.48+644402.0 1.56477e-17J152738.39+644750.6 1.64536e-17J152739.92+644643.4 1.56409e-17J152744.18+644339.9 1.61065e-17J152748.74+644825.6 1.53437e-17J152825.81+644514.3 1.52459e-17J152834.75+644643.5 1.60957e-17
< K Factor > = (1.56 +- 0.095)e-17 erg s-1cm-2/count s-1
Photometric Error~ 6%!
Full Monochromatic Ha Image of M101 - SW
Summary
• LUS intends to disentangle the individual history of each galaxy of a large sample of local galaxies– Each galaxy carries its history in its stellar populations
• Using the large FoV of OSIRIS and its TF capability• So far we are working with preliminary data &
optimising the strategy• Depend heavily on the availability of the Blue TF• Preliminary data looks promising
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