Poster
Résumé
: The
Baryon Acoustic Oscillation (BAO)
feature in the power spectrum of
galaxies can be used as a standard ruler
to probe the accelerated expansion of
the Universe. The current surveys
covering a comoving volume sufficient to
unveil the BAO scale are limited to
redshift $z \lesssim 0.6$
We study several galaxy selection
schemes aiming at building an
emission-line-galaxy (ELG) sample in the
redshift range $0.6<z<1.7$, that
would be suitable for future BAO studies
i.e. a highly biased galaxy sample.
We analyze six galaxy selections
at the redshifts 0.3, 0.5, 0.7, 0.8, 1,
1.2 using the two observables, the
angular galaxy clustering, and the weak
lensing. We combine the angular
clustering analysis with state of the
art halo occupation distribution models
to derive the properties of the haloes
these galaxies inhabit, in particular
the galaxy bias on large scales. Then a
weak lensing analysis (aperture
statistics) is performed to extract the
galaxy bias and its stochasticity as a
function of the scale.
We apply this analysis on a
dataset composed of the photometry of
the deep coadd on Stripe 82 (225
deg$^2$) made by SDSS and of WISE
infrared photometric band W1. We use the
photometric redshift of the CFHT-LS W4
T0006 and from SDSS. Both analysis on
the selections at $z=0.3$ and 0.5 are
consistent, and are in agreement with
previous studies on these tracers, which
shows our approach is valid. On the next
redshift bins, the galaxy biases
obtained using the weak lensing
observable and the bias obtained by the
clustering analysis are consistent. It
shows the galaxy populations selected
are strongly biased. Thus a survey using
such tracers of the mass field will
guarantee a high significance detection
of the BAO. This gives a strong support
for these galaxy selections to be
observed by future large spectroscopic
BAO surveys.
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Bibliographie
- Main
publications
-
Anderson, L.,
Aubourg, E., Bailey, S., et al.
2012, ArXiv e-prints Annis, J.,
Soares-Santos, M., Strauss, M. A.,
et al. 2011, ArXive-prints
- Blake,
C., Brough, S., Colless, M., et al.
2010, MNRAS , 406, 803 Cannon, R.,
Drinkwater, M., Edge, A., et al.
2006, MNRAS , 372,425
- Coupon,
J., Ilbert, O., Kilbinger, M., et
al. 2009, A&A , 500, 981 Coupon,
J., Kilbinger, M., McCracken, H. J.,
et al. 2012, A&A ,542, A5
- Eisenstein,
D. J., Annis, J., Gunn, J. E., et
al. 2001, AJ , 122, 2267 Eisenstein,
D. J., Zehavi, I., Hogg, D. W., et
al. 2005, Astrophys.J. , 633, 560
- Ilbert,
O., Arnouts, S., McCracken, H. J.,
et al. 2006, A&A , 457,841
- Jullo,
E., Rhodes, J., Kiessling, A., et
al. 2012, Astrophys. J. , 750,37
- Kilbinger,
M., Benabed, K., Cappe, O., et al.
2011, ArXiv e-prints Regnault, N.,
Conley, A., Guy, J., et al. 2009,
A&A , 506, 999 Schneider, P.,
van Waerbeke, L., Mellier, Y., et
al. 1998, A&A ,333, 767
- White,
M., Blanton, M., Bolton, A., et al.
2011, Astrophys. J. ,728, 126
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