BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES 3.5m TNG 10.4m GTC mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
THE CONTEXT PLANCK SZ CLUSTER CATALOGS PSZ1 PSZ2 Based on nominal mission data. Published in Based on nominal mission data. Published in February 2015 (Planck Collaboration XXVII) March 2013. (Planck Collaboration XXIX) New all-sky catalogue of 1653 SZ sources, New all-sky catalogue of 1227 SZ sources, the largest to date the largest to date. Confirmed galaxy clusters: 1203 Confirmed galaxy clusters: 861 Candidate clusters: 450 Candidate clusters: 366. Total=1943 Confirmed=1330 Unknown=748 BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 2 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
THE CONTEXT CLUSTER NUMBER COUNTS The cluster number counts are very useful to estimate cosmological parameter, as σ 8 and Ω m . Planck 2013 results XXIX survey selection function mass function scaling relations BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 3 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
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<latexit sha1_base64="iM358jXfnGf4hJtVvQJvJFGeaM4=">ACI3icbVDLSsQwFE19vx16SY4CNiSQfF2QiCKG4EBUeFsZY0XjVM+iC5FaT0N/wD/8KtbtyJG0H/xXTsQh3P6uSc7m5J0yVNMjYuzMwODQ8Mjo2PjE5NT0zW5ubPzFJpgW0RaISfRZyA0rG0EaJCs5SDTwKFZyG3Z3SP70FbWQSH+NdCn7Er2N5JQVHKwU1dhDkG4wVF/n+bkG3aMNbC1doJdo3c1tBvsZczyZWmdsglqduawH2k+8itRJhcOg9nF+mYgsghiF4sZ0PJain3ONUigoJs4zAykX4NHUtjHoHx895lBV3ODMeEpqCpVLQnws+JnEfG3EWhTUYcb8xfrxT/8zoZXrX8XMZphCLchFKBb1FRmhpKwN6KTUg8vLnQGVMBdcEbSkXAgrZrZDW4f39/h+ctJ0Pdvh0Xp9e68qZowskiXSIB7ZJNtknxySNhHknjySJ/LsPDgvzqvz9h0dcKqZBfILzucXYlCgPg=</latexit> <latexit sha1_base64="iM358jXfnGf4hJtVvQJvJFGeaM4=">ACI3icbVDLSsQwFE19vx16SY4CNiSQfF2QiCKG4EBUeFsZY0XjVM+iC5FaT0N/wD/8KtbtyJG0H/xXTsQh3P6uSc7m5J0yVNMjYuzMwODQ8Mjo2PjE5NT0zW5ubPzFJpgW0RaISfRZyA0rG0EaJCs5SDTwKFZyG3Z3SP70FbWQSH+NdCn7Er2N5JQVHKwU1dhDkG4wVF/n+bkG3aMNbC1doJdo3c1tBvsZczyZWmdsglqduawH2k+8itRJhcOg9nF+mYgsghiF4sZ0PJain3ONUigoJs4zAykX4NHUtjHoHx895lBV3ODMeEpqCpVLQnws+JnEfG3EWhTUYcb8xfrxT/8zoZXrX8XMZphCLchFKBb1FRmhpKwN6KTUg8vLnQGVMBdcEbSkXAgrZrZDW4f39/h+ctJ0Pdvh0Xp9e68qZowskiXSIB7ZJNtknxySNhHknjySJ/LsPDgvzqvz9h0dcKqZBfILzucXYlCgPg=</latexit> <latexit sha1_base64="iM358jXfnGf4hJtVvQJvJFGeaM4=">ACI3icbVDLSsQwFE19vx16SY4CNiSQfF2QiCKG4EBUeFsZY0XjVM+iC5FaT0N/wD/8KtbtyJG0H/xXTsQh3P6uSc7m5J0yVNMjYuzMwODQ8Mjo2PjE5NT0zW5ubPzFJpgW0RaISfRZyA0rG0EaJCs5SDTwKFZyG3Z3SP70FbWQSH+NdCn7Er2N5JQVHKwU1dhDkG4wVF/n+bkG3aMNbC1doJdo3c1tBvsZczyZWmdsglqduawH2k+8itRJhcOg9nF+mYgsghiF4sZ0PJain3ONUigoJs4zAykX4NHUtjHoHx895lBV3ODMeEpqCpVLQnws+JnEfG3EWhTUYcb8xfrxT/8zoZXrX8XMZphCLchFKBb1FRmhpKwN6KTUg8vLnQGVMBdcEbSkXAgrZrZDW4f39/h+ctJ0Pdvh0Xp9e68qZowskiXSIB7ZJNtknxySNhHknjySJ/LsPDgvzqvz9h0dcKqZBfILzucXYlCgPg=</latexit> <latexit sha1_base64="iM358jXfnGf4hJtVvQJvJFGeaM4=">ACI3icbVDLSsQwFE19vx16SY4CNiSQfF2QiCKG4EBUeFsZY0XjVM+iC5FaT0N/wD/8KtbtyJG0H/xXTsQh3P6uSc7m5J0yVNMjYuzMwODQ8Mjo2PjE5NT0zW5ubPzFJpgW0RaISfRZyA0rG0EaJCs5SDTwKFZyG3Z3SP70FbWQSH+NdCn7Er2N5JQVHKwU1dhDkG4wVF/n+bkG3aMNbC1doJdo3c1tBvsZczyZWmdsglqduawH2k+8itRJhcOg9nF+mYgsghiF4sZ0PJain3ONUigoJs4zAykX4NHUtjHoHx895lBV3ODMeEpqCpVLQnws+JnEfG3EWhTUYcb8xfrxT/8zoZXrX8XMZphCLchFKBb1FRmhpKwN6KTUg8vLnQGVMBdcEbSkXAgrZrZDW4f39/h+ctJ0Pdvh0Xp9e68qZowskiXSIB7ZJNtknxySNhHknjySJ/LsPDgvzqvz9h0dcKqZBfILzucXYlCgPg=</latexit> THE CONTEXT MASS BIAS h � � 2+ α (1 − b ) M 500 � α A ( z ) ¯ D 2 � Y 500 E � β ( z ) = Y ⇤ 10 � 4 Mpc 2 6 × 10 14 M � 0 . 7 500 = (1 − b ) M 500 = 0 . 8 +0 . 2 M HE − 0 . 1 Planck Collaboration XX BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 5 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
WHAT ABOUT THE DYNAMICAL MASS? BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 6 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
PSZ1-PSZ2 OPTICAL FOLLOW-UP: SUMMARY ~ 10000 SPECTRA BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 7 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
DYNAMICAL MASS CLUSTER IDENTIFICATION - SPECTROSCOPY • Identification of possible members in the RGB images BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 8 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
DYNAMICAL MASS CLUSTER IDENTIFICATION - SPECTROSCOPY • Identification of possible members in the RGB images • Ask for preimaging BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 9 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
DYNAMICAL MASS CLUSTER IDENTIFICATION - SPECTROSCOPY • Identification of possible members in the RGB images • Ask for preimaging • Design one mask per cluster based on the preimage, RGBs and CMDs UP TO 60 SLITLETS PER MASK BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 10 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
DYNAMICAL MASS CLUSTER IDENTIFICATION - SPECTROSCOPY • Identification of possible members in the RGB images • Ask for preimaging • Design one mask per cluster based on the preimage, RGBs and CMDs • Obtain the spectra BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 11 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
DYNAMICAL MASS CLUSTER IDENTIFICATION - SPECTROSCOPY • Identification of possible members in the RGB images • Ask for preimaging • Design one mask per cluster based on the preimage, RGBs and CMDs • Obtain the spectra • Reduce the spectra BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 12 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
DYNAMICAL MASS CLUSTER IDENTIFICATION - SPECTROSCOPY • Identification of possible members in the RGB images • Ask for preimaging • Design one mask per cluster based on the preimage, RGBs and CMDs • Obtain the spectra • Reduce the spectra • Adquire radial velocity and therefore the redshift • Using cross-correlation ( xcsao in IRAF) with Kennicutt (1992) Δ V ~ 150KM/S templates BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 13 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
DYNAMICAL MASS ESTIMATION VELOCITY DISPERSION members selection and the velocity dispersion estimation: We make a 2.5 σ clipping around the mean velocity To avoid the presence of interlopers are rejected all that galaxies with distance from the BCG (or mean of the members positions) is grater than 2.5 Mpc estimate the velocity dispersion BIAS BIASES IN THE ESTIMATION OF GALAXY CLUSTER DYNAMICAL MASSES � 14 mm Universe @ NIKA2, Grenoble 03-07 June 2019 Antonio Ferragamo
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