SDSS J081901.22+490441.4 , the SIMBAD biblio

SDSS J081901.22+490441.4 , the SIMBAD biblio (11 results) C.D.S. - SIMBAD4 rel 1.8 - 2024.04.25CEST23:19:46


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Title First 3 Authors
2003AJ....125.1817B viz 8658 242 Early-type galaxies in the Sloan Digital Sky Survey. I. The sample. BERNARDI M., SHETH R.K., ANNIS J., et al.
2005MNRAS.362....9B viz 15       D               2707 245 A sample of radio-loud active galactic nuclei in the Sloan Digital Sky Survey. BEST P.N., KAUFFMANN G., HECKMAN T.M., et al.
2010ApJ...723.1119L viz 15       D               1 1041 41 On the populations of radio galaxies with extended morphology at z < 0.3. LIN Y.-T., SHEN Y., STRAUSS M.A., et al.
2010ApJS..191..254H viz 15       D               1 20101 235 A GMBCG galaxy cluster catalog of 55,424 rich clusters from SDSS DR7. HAO J., McKAY T.A., KOESTER B.P., et al.
2012MNRAS.421.1569B viz 15       D               3 18499 511 On the fundamental dichotomy in the local radio-AGN population: accretion, evolution and host galaxy properties. BEST P.N. and HECKMAN T.M.
2012ApJ...756..116A viz 15       D               1 156 20 The lifetime and powers of FR IIs in galaxy clusters. ANTOGNINI J., BIRD J. and MARTINI P.
2014ApJ...785..104R viz 16       D               1 72334 578 redMaPPer. I. Algorithm and SDSS DR8 catalog. RYKOFF E.S., ROZO E., BUSHA M.T., et al.
2016ApJS..224....1R viz 16       D               1 670876 246 The redMaPPer galaxy cluster catalog from DES science verification data. RYKOFF E.S., ROZO E., HOLLOWOOD D., et al.
2016MNRAS.460.3669Y viz 16       D               1 7138 25 Radio luminosity function of brightest cluster galaxies. YUAN Z.S., HAN J.L. and WEN Z.L.
2018AJ....155..188L viz 16       D               1 13494 1 An analysis framework for understanding the origin of nuclear activity in low-power radio galaxies. LIN Y.-T., HUANG H.-J. and CHEN Y.-C.
2018MNRAS.478.4952F viz 16       D               1 330 4 Exploring relations between BCG and cluster properties in the SPectroscopic IDentification of eROSITA Sources survey from 0.05 <z < 0.3. FURNELL K.E., COLLINS C.A., KELVIN L.S., et al.

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