Using 11-years of OGLE V-band photometry of Q2237+0305, we measure the transverse velocity of the lens galaxy and the mean mass of its stars. We can do so because, for the first time, we fully include the random motions of the stars in the lens galaxy in the analysis of the light curves. In doing so, we are also able to correctly account for the Earth's parallax motion and the rotation of the lens galaxy, further reducing systematic errors. We measure a lower limit on the transverse speed of the lens galaxy, v_t > 338 km/s (68% confidence) and find a preferred direction to the East. The mean stellar mass estimate including a well-defined velocity prior is 0.12 <= <M/Msun> <= 1.94 at 68% confidence, with a median of 0.52 Msun. We also show for the first time that analyzing subsets of a microlensing light curve, in this case the first and second halves of the OGLE V-band light curve, give mutually consistent physical results.
A direct probe of cosmological power spectra of the peculiar velocity field and the gravitational lensing magnification from photometric redshift surveys
Statistics of Microlensing Caustic Crossings in Q~2237+0305: Peculiar Velocity of the Lens Galaxy and Accretion Disk Size
本文利用透镜系统Q~2237+0305中微透镜效应引起的焦散渡的统计特性研究透镜星系的特有速度。我们计算了一个全面的家庭的恒星质量函数的焦散交叉率，并找到一个依赖的平均焦散交叉数与有效的横向速度和平均质量，$\langle n \rangle \propto {v_{eff} / \sqrt{\langle m \rangle}}$，相当于相同质量的微透镜的情况下的理论预测。我们探索了使用$\sim$ 12年OGLE监测Q 2237+0305的4个图像测量$v_{eff}$的方法的可能性。为了确定$v_{eff}$的下限，我们保守地计算文献中确定的4个高放大倍数事件（加上我们提出的一个额外事件）中每一个的单个焦散线交叉，以获得68\%置信度的$v_{eff} \gtrsim 240\sqrt{\langle m \rangle/0.17M_\odot}\rm\,km\, s^{-1}$。从这个值和4个高放大率事件的平均$FWHM$中，我们得到了源半径（$r_s=FWHM/2.35$）的下限$r_s \gtrsim 1.4 \sqrt{\langle m \rangle/0.17M_\odot}$光日。初步确定的3个额外的焦散交叉事件导致估计$v_{eff}\simeq (493\pm 246)\sqrt{\langle m \rangle/0.17M_\odot}\rm\,km\,…
First detection of the moving lens effect with ACT and DESI LS
Perimeter Institute for Theoretical Physics；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Berkeley Center for Cosmological Physics, Department of Physics, University of California, Berkeley（加州大学伯克利分校物理系宇宙学物理中心）；Department of Physics and Astronomy, University of Pittsburgh（匹兹堡大学物理与天文学系）；Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh（匹兹堡大学匹兹堡粒子物理、天体物理和宇宙学中心）；Physics & Astronomy Department, University of Southern California（南加州大学物理与天文学系）；Kavli Institute for Particle Astrophysics and Cosmology（卡弗里粒子天体物理与宇宙学研究所）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）
The Proper Motion of Strongly Lensed Binary Neutron Star Mergers in LIGO/Virgo/Kagra can be Constrained by Measuring Doppler Induced Gravitational Wave Dephasing
Hedorah, the first yellow supergiant Kaiju star candidate at $z=3.7$ revealed by JWST behind AS1063
Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）；School of Physics and Astronomy, University of Minnesota（明尼苏达大学物理与天文学院）；STAR Institute（STAR研究所）；Université Claude Bernard Lyon 1（里昂第一大学）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；Department of Physics and Astronomy, University of Pennsylvania（宾夕法尼亚大学物理与天文学系）
