The J-PAS survey: pushing the limits of spectro-photometry
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1 The J-PAS survey: pushing the limits of spectro-photometry Silvia Bonoli For the J-PAS collaboration AYA C2-2P
2 Hyper Subaru DESI
3 Photometry - Unbiased samples Faster & cheaper Large Volumes High number density The J-PAS Survey vs. Spectroscopy - SED of targets - Precise redshifts Simulated Skies, Madrid April 2018
4 Photometry - vs. Unbiased samples Faster & cheaper Large Volumes High number density - SED of targets - Precise redshifts Spectro-Photometry COMBO-17 Spectroscopy
5 Spectro-Photometry
6 The OAJ observatory M1 (Ø) = 2.55 m FoV (Ø) = 3 deg = 476 mm at FP Etendue = 27.5 m2deg2 Currently equipped with the pathfinder camera M1 (Ø) = 0.8 m FoV (Ø)) = 2 deg
7 JPCam T80Cam
8 JPCam T80Cam
9 The camera JPCam 1.2 Giga pixels (14 CCD of 9200x9200) 0.22 arcsec/pixel 4.5 deg2
10 The camera JPCam 1.2 Giga pixels (14 CCD of 9200x9200) 0.22 arcsec/pixel 4.5 deg2
11 The filter system - 54 NB filters (FWHM~145Å; Dl~10nm) From 3785Å to 9100Å - 1 Blue MB filter (FWHM~260Å; lc~3600å) - 1 Red BB filter (FWHM~620Å; lc~9500å) - Sloan u, g, r Pseudo-spectrum (R~50) for every pixel of the sky 5σ 3 aperture
12 The camera + filters Tray 2 Tray 1 Tray 4 The J-PAS Survey Tray 3 Tray BB Simulated Skies, Madrid April 2018
13 The filter system z=1 Photo-z precision as good as 0.003(1+z) z~3.5 The J-PAS Survey Simulated Skies, Madrid April 2018
14 Footprint Expected survey speed: ~ 1000 deg² /yr
15 Cosmology experiments Type Ia Supernovae ~4000 SNIa - exposure cadence - redshift from SN SED or host galaxy - characterization of environment - 700k clusters with more than 10 members down to ~few 1013 Msun Clusters The J-PAS Survey - Combine lensing and optical richness for mass calibration - 90M galaxies (LRG, ELG) with photo-z precision of 0.3% - 2M QSOs - ks LAE Clustering - Optimization of BB observations in the best nights - Redshift precision for lenses and background galaxies Lensing Simulated Skies, Madrid April 2018
16 Cosmology experiments Type Ia Supernovae ~4000 SNIa - exposure cadence - redshift from SN SED or host galaxy - characterization of environment - 700k clusters with more than 10 members down to ~few 1013 Msun Clusters The J-PAS Survey - Combine lensing and optical richness for mass calibration - 90M galaxies (LRG, ELG) with photo-z precision of 0.3% - 2M QSOs - ks LAE Clustering - Optimization of BB observations in the best nights - Redshift precision for lenses and background galaxies Lensing Simulated Skies, Madrid April 2018
17 Cosmology experiments Type Ia Supernovae LRG ELG QSO Clusters The J-PAS Survey ~4000 SNIa - exposure cadence - redshift from SN SED or host galaxy - characterization of environment - 700k clusters with more than 10 members down to ~few 1013 Msun - Combine lensing and optical richness for mass calibration Photo-z error Red Blue 0.3% 17M 73M 1% 64M 200M 3% 100M 285M - 90M galaxies (LRG, ELG) with photo-z precision of 0.3% - 2M QSOs - ks LAE - Very good median the OAJ J-PAS DESI - BB images taken EUCLID during best nights - Redshift precision for lenses and background galaxies Clustering Raul Abramo s forecasts Lensing Simulated Skies, Madrid April 2018
18 Cosmology experiments Type Ia Supernovae ~4000 SNIa - exposure cadence - redshift from SN SED or host galaxy - characterization of environment - 90M galaxies (LRG, ELG) with photo-z precision of 0.3% - 2M QSOs - ks LAE - 700k clusters with more than 10 members down to ~few 1013 Msun the OAJ - BB images taken during best nights - Redshift precision for lenses and background galaxies Clustering WEAVE-QSO survey: Follow-up of 0.5M- QSOs at z>2.2 Very good median Clusters The J-PAS Survey - Combine lensing and optical richness for mass calibration Lensing Pieri et al., 2016 Simulated Skies, Madrid April 2018
19 Cosmology experiments Ascaso et al. Type Ia Supernovae ~4000 SNIa - exposure cadence - redshift from SN SED or host galaxy - characterization of environment - 700k clusters with more than 10 members down to ~few 1013 Msun Clusters - Combine lensing and optical richness for mass calibration Synergy with erosita (DE) - 90M galaxies (LRG, ELG) with photo-z precision of 0.3% - 2M QSOs - ks LAE - Very good median the OAJ - BB images taken during best nights - Redshift precision for lenses and background galaxies BAO Lensing
20 Galaxy evolution z~1 z~3
21 Galactic science Characterize the basic physical properties of the observed stars (temperature, gravity, metallicity ) Discovery and characterization of stellar populations of ultra dwarf galaxies RR-Lyrae variable stars should be able to be observed up to ~200 kpc. Used as tracers of galactic subsystems Tidal streams and low surface brightness structures White Dwarfs - age indicators of the group they belong to PNe provide important information to study low-mass stars evolution and the early chemical composition of the Galaxy Search for ultra metal-poor stars (only ~100 already known with [Fe/H]<-3 up to now) The J-PAS Survey Characterization of binary (and multiple) stars (e.g, CVs, AM CVs) Simulated Skies, Madrid April 2018
22 Time-line for J-PAS Current time-line: - Early/Mid 2018: Start of mini-jpas - Final assembly and fine-tuning of JPCam - Mid/End 2018: Coating of the T250 mirror - Beginning 2019: Installation of JPCam and Start of J-PAS The J-PAS Survey Simulated Skies, Madrid April 2018
23 Time-line for J-PAS Current time-line: - Early/Mid 2018: Start of mini-jpas - Final assembly and fine-tuning of JPCam - Mid/End 2018: Coating of the T250 mirror - Beginning 2019: Installation of JPCam and Start of J-PAS mini-jpas (~3 deg2 at full-depth with all the filters on the AEGIS field) Goals: - telescope final testing (e.g., actuator system) - data-reduction pipeline testing - scientific-analysis pipelines testing - first scientific results
24 Collaboration board: Javier Cenarro (CEFCA) Renato Dupke (ON) Laerte Sodre (USP) Jose Vilchez (IAA-CSIC) Scientific coordinators: Silvia Bonoli (CEFCA) Renato Dupke (ON)
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