Cosmology from Supernova Magnification Maps

High-z Type Ia supernovae are expected to be gravitationally lensed by the foreground distribution of large-scale structure. The resulting magnification of supernovae is statistically measurable, and the angular correlation of the magnification pattern directly probes the integrated mass density along the line of sight. Measurements of the cosmic magnification of supernovae therefore complement measurements of galaxy shear in providing a direct measure of the clustering of the dark matter. As the surface density of supernovae is typically much smaller than that of sheared galaxies, the two-point correlation function of lensed Type Ia supernovae suffers from significantly increased shot noise. Nevertheless, we find that the magnification map of a large sample of supernovae provides an important cosmological tool. For example, a search over 20 deg2 over 5 years leading to a sample of ~10,000 supernovae would measure the angular power spectrum of cosmic magnification with a cumulative signal-to-noise ratio of ~20. This detection can be further improved once the supernova distance measurements are cross-correlated with measurements of the foreground galaxy distribution. The magnification maps made using supernovae can be used for important cross-checks with traditional lensing shear statistics obtained in the same fields and can help to control systematics.

[1]  U. Pen,et al.  Mapping dark matter with cosmic magnification. , 2005, Physical review letters.

[2]  T. Totani,et al.  Deciphering the Cosmic Star Formation History and the Nature of Type Ia Supernovae with Future Supernova Surveys , 2005, astro-ph/0505312.

[3]  Daniel E. Holz,et al.  Using Gravitational-Wave Standard Sirens , 2005, astro-ph/0504616.

[4]  A. Myers,et al.  Detection of Cosmic Magnification with the Sloan Digital Sky Survey , 2005, astro-ph/0504510.

[5]  B. M'enard,et al.  Revisiting the magnification of type Ia supernovae with SDSS , 2004, astro-ph/0407023.

[6]  D. Huterer,et al.  Uncorrelated estimates of dark energy evolution , 2004, astro-ph/0404062.

[7]  D. Holz,et al.  Safety in Numbers: Gravitational Lensing Degradation of the Luminosity Distance-Redshift Relation , 2004, astro-ph/0412173.

[8]  Yun Wang Observational signatures of the weak lensing magnification of supernovae , 2004, astro-ph/0406635.

[9]  M. Lombardi,et al.  Mass-sheet degeneracy: Fundamental limit on the cluster mass reconstruction from statistical (weak) lensing , 2004, astro-ph/0405357.

[10]  Stefano Casertano,et al.  Type Ia Supernova Discoveries at z > 1 from the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Energy Evolution , 2004, astro-ph/0402512.

[11]  Adam G. Riess,et al.  Twenty-Three High-Redshift Supernovae from the Institute for Astronomy Deep Survey: Doubling the Supernova Sample at z > 0.7 , 2004 .

[12]  A. Cooray Lensing studies with diffuse backgrounds , 2003, astro-ph/0309301.

[13]  Michael C. Liu,et al.  23 High Redshift Supernovae from the IfA Deep Survey: Doubling the SN Sample at z>0.7 , 2003, astro-ph/0310843.

[14]  E. Rozo,et al.  Primordial gravity waves and weak lensing. , 2003, Physical review letters.

[15]  B. Jain Magnification Effects as Measures of Large-Scale Structure , 2002, astro-ph/0208515.

[16]  R. Sheth,et al.  Halo Models of Large Scale Structure , 2002, astro-ph/0206508.

[17]  J. Frieman,et al.  Corrective Lenses for High-Redshift Supernovae , 2002, astro-ph/0206339.

[18]  Y. Jing,et al.  Intrinsic correlation of halo ellipticity and its implications for large-scale weak lensing surveys , 2002, astro-ph/0206098.

[19]  I. Hook,et al.  Accepted for publication in The Astrophysical Journal LPNHE 02-02 The distant Type Ia supernova rate , 2002 .

[20]  D. Holz,et al.  A Universal Probability Distribution Function for Weak-lensing Amplification , 2002, astro-ph/0204169.

[21]  A. Cooray,et al.  Second-Order Corrections to Weak Lensing by Large-Scale Structure , 2002, astro-ph/0202411.

[22]  D. Huterer,et al.  Weak lensing and dark energy , 2001, astro-ph/0106399.

[23]  A. Heavens,et al.  Intrinsic correlation of galaxy shapes: implications for weak lensing measurements , 2000, astro-ph/0005269.

[24]  A. Cooray,et al.  Weak Lensing by Large-Scale Structure: A Dark Matter Halo Approach , 2000, The Astrophysical journal.

[25]  Yun Wang,et al.  Flux-averaging Analysis of Type Ia Supernova Data , 1999, astro-ph/9907405.

[26]  Max Tegmark,et al.  Weak Lensing: Prospects for Measuring Cosmological Parameters , 1998, astro-ph/9811168.

[27]  M. Bartelmann,et al.  Gravitational lensing of type Ia supernovae by galaxy clusters , 1997, astro-ph/9708120.

[28]  D. Holz,et al.  A New method for determining cumulative gravitational lensing effects in inhomogeneous universes , 1997, astro-ph/9708036.

[29]  N. Kaiser Weak Lensing and Cosmology , 1996, astro-ph/9610120.

[30]  David W. Hogg,et al.  Deep Optical Galaxy Counts with the Keck Telescope , 1995, astro-ph/9506095.

[31]  N. Kaiser,et al.  Mapping the dark matter with weak gravitational lensing , 1993 .

[32]  I. Shapiro,et al.  On model-dependent bounds on H(0) from gravitational images Application of Q0957 + 561A,B , 1985 .