text: 155,8,1377983221946839042,1912298966,Dr. L. C. Mayorga,"New paper was accepted with the fabulous @exowanderer and @kevinbstevenson! <LINK>  We observed a secondary eclipse of WASP-43b with HST in the optical! 1/10 <LINK> WASP-43b is particularly exciting because modeling showed that it had the potential for MgSiO3 clouds or MnS clouds, which have very different reflected light properties. 2/10 <LINK> We asked for a whole phase curve (24 orbits), but only got awarded an eclipse (4 orbits). The TAC strikes again! We suspected that MgSiO3 clouds would be inhomogeneous because they could be cold trapped (below the observable photosphere). 3/10 <LINK> Instead of staring at a motionless star, we used a new mode for HST WFC3/UVIS that “scans” the star across the detector, allowing us to build up lots of signal without saturating our bright target. 4/10 <LINK> To analyze this new HST mode, @exowanderer built Arctor! <LINK> a new scanning extraction and analysis pipeline! 5/10 <LINK> Here’s what we got!!! No, April Fools. The TAC was probably onto something… 6/10 <LINK> We place a 67ppm 3-sigma upper limit on the eclipse depth, a geometric albedo limit (in F350LP) at 0.06. My modeling suggests that only the most lofted cloud case scenario can escape a cold trap at the deepest layer of the atmosphere on the day side. 7/10 <LINK> From nightside observations, we can be pretty sure that clouds there were limiting the depth that we could probe in the atmosphere. This means that the clouds on WASP-43b are inhomogeneously distributed! 8/10 <LINK> Model predictions suggest that there is a correlation between planet equilibrium temperature and where this cold trap starts to occur -&gt; causing an albedo drop, because MgSiO3 is normally really bright! (from @V_Parmentier work) 9/10 <LINK> With WASP-43b proving to be the darkest of worlds, it’s now time to study other exoplanets at different temperatures and gravities to figure out where and how MgSiO3 clouds form. See the paper for more! <LINK> 10/10 <LINK>",https://arxiv.org/abs/2103.16676,"Optical, reflected light eclipse observations provide a direct probe of the exoplanet scattering properties, such as from aerosols. We present here the photometric, reflected light observations of WASP-43b using the HST WFC3/UVIS instrument with the F350LP filter (346-822nm) encompassing the entire optical band. This is the first reflected light, photometric eclipse using UVIS in scanning mode; as such we further detail our scanning extraction and analysis pipeline Arctor. Our HST WFC3/UVIS eclipse light curve for WASP-43 b derived a 3-{\sigma} upper limit of 67 ppm on the eclipse depth, which implies that WASP-43b has a very dark dayside atmosphere. With our atmospheric modeling campaign, we compared our reflected light constraints with predictions from global circulation and cloud models, benchmarked with HST and Spitzer observations of WASP-43b. We infer that we do not detect clouds on the dayside within the pressure levels probed by HST WFC3/UVIS with the F350LP filter (P > 1 bar). This is consistent with the GCM predictions based on previous WASP-43b observations. Dayside emission spectroscopy results from WASP-43b with HST and Spitzer observations are likely to not be significantly affected by contributions from cloud particles. ",The Dark World: A Tale of WASP-43b in Reflected Light with HST WFC3/UVIS,10,"['New paper was accepted with the fabulous @exowanderer and @kevinbstevenson! <LINK> \n\nWe observed a secondary eclipse of WASP-43b with HST in the optical! 1/10 <LINK>', 'WASP-43b is particularly exciting because modeling showed that it had the potential for MgSiO3 clouds or MnS clouds, which have very different reflected light properties. 2/10 https://t.co/WpN5lmKpT2', 'We asked for a whole phase curve (24 orbits), but only got awarded an eclipse (4 orbits). The TAC strikes again! We suspected that MgSiO3 clouds would be inhomogeneous because they could be cold trapped (below the observable photosphere). 3/10 https://t.co/kXaUzLkMSJ', 'Instead of staring at a motionless star, we used a new mode for HST WFC3/UVIS that “scans” the star across the detector, allowing us to build up lots of signal without saturating our bright target. 4/10 https://t.co/4CHRWhdlQF', 'To analyze this new HST mode, @exowanderer built Arctor! https://t.co/KDGKqf9rSX a new scanning extraction and analysis pipeline! 5/10 https://t.co/plOPCn5R5e', 'Here’s what we got!!! No, April Fools. The TAC was probably onto something… 6/10 https://t.co/DnMvXc8Q7c', 'We place a 67ppm 3-sigma upper limit on the eclipse depth, a geometric albedo limit (in F350LP) at 0.06. My modeling suggests that only the most lofted cloud case scenario can escape a cold trap at the deepest layer of the atmosphere on the day side. 7/10 https://t.co/3yjYwibWDU', 'From nightside observations, we can be pretty sure that clouds there were limiting the depth that we could probe in the atmosphere. This means that the clouds on WASP-43b are inhomogeneously distributed! 8/10 https://t.co/Wd2jFMBv4a', 'Model predictions suggest that there is a correlation between planet equilibrium temperature and where this cold trap starts to occur -&gt; causing an albedo drop, because MgSiO3 is normally really bright! (from @V_Parmentier work) 9/10 https://t.co/aaT6RRWipw', 'With WASP-43b proving to be the darkest of worlds, it’s now time to study other exoplanets at different temperatures and gravities to figure out where and how MgSiO3 clouds form. See the paper for more! https://t.co/OkthjJXNoN 10/10 https://t.co/4FxUmj8uxZ']",21,03,1967