J-PAS: low-resolution (R 50) spectroscopy over 8000 deg 2

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1 J-PAS: low-resolution (R 50) spectroscopy over 8000 deg 2 C. López-Sanjuan J. Cenarro, L. A. Díaz-García, J. Varela, K. Viironen, & the J-PAS team Centro de Estudio de Física del Cosmos de Aragón 10th July 2014 / IAUS 309 / Wien

2 J-PAS: A next generation photometric survey J-PAS : Javalambre - Physics of the accelerated universe Astrophysical Survey (Benítez et al [ArXiv: ]) J-PAS will map 8000 deg 2 of the northern sky with 54 narrow-band filters ( 14 nm) + 2 medium-bands at the blue and red ends. J-PAS (j-pas.org) will be carry out in the OAJ, a new astronomical facility located in Teruel, Spain.

3 J-PAS: low-resolution (R 50) spectroscopy F λ (Arbitrary units) Residuals M32 Spectrum Best-fitting model M32 synthetic photometry λ( A) J-PAS will provide low-resolution (R 50) photo-spectra. Very accurate photometric redshifts with z/(1 + z) 0.3%, cosmology, galaxy evolution, and IFU (i.e., spatially resolved) science.

4 J-PAS: 2D stellar populations BCG galaxy at z = observed with medium-band photometry (ALHAMBRA survey, Moles+08; only 20 filters in the optical). Both age and metallicity gradients are observed.

5 J-PAS: 2D stellar populations BCG galaxy at z = observed with medium-band photometry (ALHAMBRA survey, Moles+08; only 20 filters in the optical). Both age and metallicity gradients are observed.

6 J-PAS: 2D star formation rate CALIFA: Hα emission The star forming regions traced by emission lines, such as Hα or [OII], will be detected with J-PAS, and the star formation rate estimated.

7 J-PAS: 2D star formation rate J-PAS: F660 - r CALIFA: Hα emission The star forming regions traced by emission lines, such as Hα or [OII], will be detected with J-PAS, and the star formation rate estimated.

8 J-PAS: Field-of-view and environment CALIFA Sánchez+12 SAURON instrument Bacon+01

9 J-PAS: Field-of-view and environment CALIFA Sánchez+12 SAURON instrument Bacon+01

10 Summary J-PAS as a low-resulition spectrograph J-PAS will provide low-resolution (R 50) photo-spectra of a hundred million galaxies to r 23.5 by J-PAS will complement high-resolution IFSs and permit the study of 2D stellar populations, star forming regions, and the environment of local Universe galaxies. J-PAS is a perfect reference for flux calibration of IFSs spectra. J-PLUS and S-PLUS will survey the northern and the southern sky with 5 SDSS + 7 narrow-band filters (including Hα and [OII]) in the next four years. Thank you for your attention. Let schnitzel!!

11 Summary J-PAS as a low-resulition spectrograph J-PAS will provide low-resolution (R 50) photo-spectra of a hundred million galaxies to r 23.5 by J-PAS will complement high-resolution IFSs and permit the study of 2D stellar populations, star forming regions, and the environment of local Universe galaxies. J-PAS is a perfect reference for flux calibration of IFSs spectra. J-PLUS and S-PLUS will survey the northern and the southern sky with 5 SDSS + 7 narrow-band filters (including Hα and [OII]) in the next four years. Thank you for your attention. Let schnitzel!!

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