在大型星系周围绘制气体：DES Y3星系和Compton- $ Y $ - SPT和Planck的互相关

论文标题

在大型星系周围绘制气体：DES Y3星系和Compton- $ Y $ - SPT和Planck的互相关

Mapping gas around massive galaxies: cross-correlation of DES Y3 galaxies and Compton-$y$-maps from SPT and Planck

论文作者

Sánchez, J., Omori, Y., Chang, C., Bleem, L. E., Crawford, T., Drlica-Wagner, A., Raghunathan, S., Zacharegkas, G., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Avila, S., Baxter, E., Bechtol, K., Benson, B. A., Bernstein, G. M., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Campos, A., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C. L., Chen, A., Choi, A., Chown, R., Costanzi, M., Crites, A. T., Crocce, M., da Costa, L. N., Pereira, M. E. S., de Haan, T., De Vicente, J., DeRose, J., Desai, S., Diehl, H. T., Dobbs, M. A., Dodelson, S., Doel, P., Elvin-Poole, J., Everett, W., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gatti, M., George, E. M., Gerdes, D. W., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Hinton, S. R., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., James, D. J., Knox, L., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, A. T., Luong-Van, D., MacCrann, N., Marshall, J. L., McCullough, J., McMahon, J. J., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mocanu, L., Mohr, J. J., Muir, J., Myles, J., Natoli, T., Padin, S., Palmese, A., Pandey, S., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Pryke, C., Raveri, M., Reichardt, C. L., Rodriguez-Monroy, M., Ross, A. J., Ruhl, J. E., Rykoff, E., Sánchez, C., Sanchez, E., Scarpine, V., Schaffer, K. K., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Smith, M., Soares-Santos, M., Staniszewski, Z., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vieira, J. D., Vincenzi, M., Weaverdyck, N., Williamson, R., Yanny, B., Yin, B.

论文摘要

我们使用来自South Pole望远镜（SPT）和{\ it Planck}任务的数据生成的compton-$ $ $ thaps在数据的前三年中测量的星系的位置。我们将这种互相关测量与星系自动相关建模，以限制宇宙中气体的分布。我们使用大规模信息，使用大规模信息，我们使用大规模信息来测量静水体质量偏置或等效地，等效地，等效地，平均光晕偏置给电压$ \ langle b_ {h} p_ {e} \ rangle $。我们发现$ \ langle b_ {h} p_ {e} \ rangle $ be $ [0.16^{+0.03} _ { - 0.04}，0.28^{+0.04} _ { - 0.05}，0.45^{+0.06} _ { - 0.10} ，0.54^{+0.08} _ { - 0.07}，0.61^{+0.08} _ { - 0.06}，0.63^{+0.07} _ { - 0.08}] $ Mev cm $^{ - 3} $在RedShifts $ Z \ SIM [0.30，0.46，0.62,0.77，0.89，0.97] $。这些值与以前存在的Redshift范围内的测量值一致。我们还使用小规模信息来限制平均气体轮廓，这是由SPT数据的高分辨率启用的。我们将测量结果与基于宇宙owl的流体动力学模拟的不同参数化剖面进行了比较。我们发现我们的数据与假定AGN加热温度为$ 10^{8.5} $ K的模拟一致，但与假定AGN加热温度为$ 10^{8.0} $ K的模型不兼容。这些比较表明，与Galaxies Halos的$ R_ {500C} $内的模拟相比，数据更喜欢电子压力值。

We cross-correlate positions of galaxies measured in data from the first three years of the Dark Energy Survey with Compton-$y$-maps generated using data from the South Pole Telescope (SPT) and the {\it Planck} mission. We model this cross-correlation measurement together with the galaxy auto-correlation to constrain the distribution of gas in the Universe. We measure the hydrostatic mass bias or, equivalently, the mean halo bias-weighted electron pressure $\langle b_{h}P_{e}\rangle$, using large-scale information. We find $\langle b_{h}P_{e}\rangle$ to be $[0.16^{+0.03}_{-0.04},0.28^{+0.04}_{-0.05},0.45^{+0.06}_{-0.10},0.54^{+0.08}_{-0.07},0.61^{+0.08}_{-0.06},0.63^{+0.07}_{-0.08}]$ meV cm$^{-3}$ at redshifts $z \sim [0.30, 0.46, 0.62,0.77, 0.89, 0.97]$. These values are consistent with previous work where measurements exist in the redshift range. We also constrain the mean gas profile using small-scale information, enabled by the high-resolution of the SPT data. We compare our measurements to different parametrized profiles based on the cosmo-OWLS hydrodynamical simulations. We find that our data are consistent with the simulation that assumes an AGN heating temperature of $10^{8.5}$K but are incompatible with the model that assumes an AGN heating temperature of $10^{8.0}$K. These comparisons indicate that the data prefer a higher value of electron pressure than the simulations within $r_{500c}$ of the galaxies' halos.

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