Author: "Poleski, Radosław" / Publication Type: Electronic Resources - Searchworks@Jio Institute Digital Library Search Results

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77 results on '"Poleski, Radosław"'

1. OGLE-2018-BLG-0971, MOA-2023-BLG-065, and OGLE-2023-BLG-0136: Microlensing events with prominent orbital effects

Author: Han, Cheongho, Udalski, Andrzej, Bond, Ian A., Lee, Chung-Uk, Gould, Andrew, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Yang, Hongjing, Zang, Weicheng, Cha, Sang-Mok, Kim, Doeon, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Mróz, Mateusz J., Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Fujii, Hirosame, Fukui, Akihiko, Hamada, Ryusei, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Kirikawa, Rintaro, Koshimoto, Naoki, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Olmschenk, Greg, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Sumi, Takahiro, Suzuki, Daisuke, Tomoyoshi, Mio, Tristram, Paul J., Vandorou, Aikaterini, Yama, Hibiki, Yamashita, Kansuke, Han, Cheongho, Udalski, Andrzej, Bond, Ian A., Lee, Chung-Uk, Gould, Andrew, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Yang, Hongjing, Zang, Weicheng, Cha, Sang-Mok, Kim, Doeon, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Mróz, Mateusz J., Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Fujii, Hirosame, Fukui, Akihiko, Hamada, Ryusei, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Kirikawa, Rintaro, Koshimoto, Naoki, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Olmschenk, Greg, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Sumi, Takahiro, Suzuki, Daisuke, Tomoyoshi, Mio, Tristram, Paul J., Vandorou, Aikaterini, Yama, Hibiki, and Yamashita, Kansuke
Abstract: We undertake a project to reexamine microlensing data gathered from high-cadence surveys. The aim of the project is to reinvestigate lensing events with light curves exhibiting intricate anomaly features associated with caustics, yet lacking prior proposed models to explain these features. Through detailed reanalyses considering higher-order effects, we identify that accounting for orbital motions of lenses is vital in accurately explaining the anomaly features observed in the light curves of the lensing events OGLE-2018-BLG-0971, MOA-2023-BLG-065, and OGLE-2023-BLG-0136. We estimate the masses and distances to the lenses by conducting Bayesian analyses using the lensing parameters of the newly found lensing solutions. From these analyses, we identify that the lenses of the events OGLE-2018-BLG-0971 and MOA-2023-BLG-065 are binaries composed of M dwarfs, while the lens of OGLE-2023-BLG-0136 is likely to be a binary composed of an early K-dwarf primary and a late M-dwarf companion. For all lensing events, the probability of the lens residing in the bulge is considerably higher than that of it being located in the disk., Comment: 11 pages, 13 figures, 6 tables
Published: 2024

2. Virial Black Hole Masses for AGNs behind the Magellanic Clouds

Author: Panda, Swayamtrupta, Kozłowski, Szymon, Gromadzki, Mariusz, Wrona, Marcin, Iwanek, Patryk, Udalski, Andrzej, Szymański, Michał K., Soszyński, Igor, Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Skowron, Jan, Poleski, Radosław, Mróz, Przemek, Skowron, Dorota M., Rybicki, Krzysztof, Mróz, Mateusz, Panda, Swayamtrupta, Kozłowski, Szymon, Gromadzki, Mariusz, Wrona, Marcin, Iwanek, Patryk, Udalski, Andrzej, Szymański, Michał K., Soszyński, Igor, Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Skowron, Jan, Poleski, Radosław, Mróz, Przemek, Skowron, Dorota M., Rybicki, Krzysztof, and Mróz, Mateusz
Abstract: We use the spectroscopic data collected by the Magellanic Quasars Survey (MQS) as well as the photometric V- and I-band data from the Optical Gravitational Lensing Experiment (OGLE) to measure the physical parameters for active galactic nuclei (AGNs) located behind the Magellanic Clouds. The flux-uncalibrated MQS spectra were obtained with the 4-m Anglo-Australian Telescope and the AAOmega spectroscope (R=1300) in a typical ~1.5-hour visit. They span a spectral range of 3700-8500 Angstroms and have S/N ratios in a range of 3-300. We report the discovery and observational properties of 161 AGNs in this footprint, which expands the total number of spectroscopically confirmed AGNs by MQS to 919. After converting the OGLE mean magnitudes to the monochromatic luminosities at 5100 Angstroms, 3000 Angstroms, and 1350 Angstroms, we reliably measured the black hole masses for 165 out of 919 AGNs. The remaining physical parameters we provide are the bolometric luminosities and the Eddington ratios. A fraction of these AGNs have been observed by the OGLE survey since 1997 (all of them since 2001), enabling studies of correlations between their variability and physical parameters., Comment: 15 pages, 8 figures, 8 tables, accepted for publication in The Astrophysical Journal Supplement Series
Published: 2024

3. Verification of Hypervelocity Bulge Red Clump Stars

Author: Wojtkowska, Gabriela, Poleski, Radosław, Wojtkowska, Gabriela, and Poleski, Radosław
Abstract: We verify candidate hypervelocity red clump stars located in the Galactic bulge that were selected based on the VVV and the Gaia DR2 data by Luna et al. (2019). To do so, we analyze data from the OGLE-IV survey: difference images and astrometric time series. We have data for 30 stars out of 34 hypervelocity candidates. We confirmed high proper motion of only one of these stars and find out that it is a nearby one, hence, not hypervelocity. To sum up, we do not confirm the candidate stars as hypervelocity ones. Hence, we disprove the production rate of hypervelocity red clump stars by the central supermassive black hole provided by Luna et al. (2019)., Comment: accepted by AAS Journals
Published: 2024

4. OGLE-2023-BLG-0836L: The sixth microlensing planet in a binary stellar system

Author: Han, Cheongho, Udalski, Andrzej, Jung, Youn Kil, Gould, Andrew, Kim, Doeon, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Yang, Hongjing, Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Mróz, Mateusz J., Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Udalski, Andrzej, Jung, Youn Kil, Gould, Andrew, Kim, Doeon, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Yang, Hongjing, Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Mróz, Mateusz J., Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: Light curves of microlensing events occasionally deviate from the smooth and symmetric form of a single-lens single-source event. While most of these anomalous events can be accounted for by employing a binary-lens single-source (2L1S) or a single-lens binary-source (1L2S) framework, it is established that a small fraction of events remain unexplained by either of these interpretations. We carry out a project in which data collected by high-cadence microlensing surveys were reinvestigated with the aim of uncovering the nature of anomalous lensing events with no proposed 2L1S or 1L2S models. From the project, we find that the anomaly appearing in the lensing event OGLE-2023-BLG-0836 cannot be explained by the usual interpretations and conduct a comprehensive analysis of the event. From thorough modeling of the light curve under sophisticated lens-system configurations, we have arrived at the conclusion that a triple-mass lens system is imperative to account for the anomaly features observed in the lensing light curve. From the Bayesian analysis using the measured observables of the event time scale and angular Einstein radius, we determine that the least massive component of the lens has a planetary mass of $4.36^{+2.35}_{-2.18}~M_{\rm J}$. This planet orbits within a stellar binary system composed of two stars with masses $0.71^{+0.38}_{-0.36}~M_\odot$ and $0.56^{+0.30}_{-0.28}~M_\odot$. This lensing event signifies the sixth occurrence of a planetary microlensing system in which a planet belongs to a stellar binary system., Comment: 11 pages, 12 figures
Published: 2024

5. KMT-2023-BLG-0416, KMT-2023-BLG-1454, KMT-2023-BLG-1642: Microlensing planets identified from partially covered signals

Author: Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Zang, Weicheng, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Yang, Hongjing, Cha, Sang-Mok, Kim, Doeon, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Mróz, Mateusz, Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Zang, Weicheng, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Yang, Hongjing, Cha, Sang-Mok, Kim, Doeon, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, and Mróz, Mateusz
Abstract: We investigate the 2023 season data from high-cadence microlensing surveys with the aim of detecting partially covered short-term signals and revealing their underlying astrophysical origins. Through this analysis, we ascertain that the signals observed in the lensing events KMT-2023-BLG-0416, KMT-2023-BLG-1454, and KMT-2023-BLG-1642 are of planetary origin. Considering the potential degeneracy caused by the partial coverage of signals, we thoroughly investigate the lensing-parameter plane. In the case of KMT-2023-BLG-0416, we have identified two solution sets, one with a planet-to-host mass ratio of $q\sim 10^{-2}$ and the other with $q\sim 6\times 10^{-5}$, within each of which there are two local solutions emerging due to the inner-outer degeneracy. For KMT-2023-BLG-1454, we discern four local solutions featuring mass ratios of $q\sim (1.7-4.3)\times 10^{-3}$. When it comes to KMT-2023-BLG-1642, we identified two locals with $q\sim (6-10)\times 10^{-3}$ resulting from the inner-outer degeneracy. We estimate the physical lens parameters by conducting Bayesian analyses based on the event time scale and Einstein radius. For KMT-2023-BLG-0416L, the host mass is $\sim 0.6~M_\odot$, and the planet mass is $\sim (6.1-6.7)~M_{\rm J}$ according to one set of solutions and $\sim 0.04~M_{\rm J}$ according to the other set of solutions. KMT-2023-BLG-1454Lb has a mass roughly half that of Jupiter, while KMT-2023-BLG-1646Lb has a mass in the range of between 1.1 to 1.3 times that of Jupiter, classifying them both as giant planets orbiting mid M-dwarf host stars with masses ranging from 0.13 to 0.17 solar masses., Comment: 12 pages, 16 figures, 6 tables
Published: 2024

6. Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Sub-Prime Field Planets

Author: Shin, In-Gu, Yee, Jennifer C., Zang, Weicheng, Han, Cheongho, Yang, Hongjing, Gould, Andrew, Lee, Chung-Uk, Udalski, Andrzej, Sumi, Takahiro, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Abe, Fumio, Bando, Ken, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Bond, Ian A., Fujii, Hirosane, Fukui, Akihiko, Hamada, Ryusei, Hamada, Shunya, Hamasaki, Naoto, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Kirikawa, Rintaro, Koshimoto, Naoki, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Nagai, Tutumi, Nunota, Kansuke, Olmschenk, Greg, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Suzuki, Daisuke, Tomoyoshi, Mio, Tristram, Paul . J., Vandorou, Aikaterini, Yama, Hibiki, Yamashita, Kansuke, Shin, In-Gu, Yee, Jennifer C., Zang, Weicheng, Han, Cheongho, Yang, Hongjing, Gould, Andrew, Lee, Chung-Uk, Udalski, Andrzej, Sumi, Takahiro, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Abe, Fumio, Bando, Ken, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Bond, Ian A., Fujii, Hirosane, Fukui, Akihiko, Hamada, Ryusei, Hamada, Shunya, Hamasaki, Naoto, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Kirikawa, Rintaro, Koshimoto, Naoki, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Nagai, Tutumi, Nunota, Kansuke, Olmschenk, Greg, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Suzuki, Daisuke, Tomoyoshi, Mio, Tristram, Paul . J., Vandorou, Aikaterini, Yama, Hibiki, and Yamashita, Kansuke
Abstract: Following Shin et al. (2023b), which is a part of the Systematic KMTNet Planetary Anomaly Search series (i.e., a search for planets in the 2016 KMTNet prime fields), we conduct a systematic search of the 2016 KMTNet sub-prime fields using a semi-machine-based algorithm to identify hidden anomalous events missed by the conventional by-eye search. We find four new planets and seven planet candidates that were buried in the KMTNet archive. The new planets are OGLE-2016-BLG-1598Lb, OGLE-2016-BLG-1800Lb, MOA-2016-BLG-526Lb, and KMT-2016-BLG-2321Lb, which show typical properties of microlensing planets, i.e., giant planets orbit M dwarf host stars beyond their snow lines. For the planet candidates, we find planet/binary or 2L1S/1L2S degeneracies, which are an obstacle to firmly claiming planet detections. By combining the results of Shin et al. (2023b) and this work, we find a total of nine hidden planets, which is about half the number of planets discovered by eye in 2016. With this work, we have met the goal of the systematic search series for 2016, which is to build a complete microlensing planet sample. We also show that our systematic searches significantly contribute to completing the planet sample, especially for planet/host mass ratios smaller than $10^{-3}$, which were incomplete in previous by-eye searches of the KMTNet archive., Comment: 63 pages, 16 Tables, 19 Figures, Submitted in the AAS journal
Published: 2024

7. OGLE-2019-BLG-0825: Constraints on the Source System and Effect on Binary-lens Parameters arising from a Five Day Xallarap Effect in a Candidate Planetary Microlensing Event

Author: Satoh, Yuki K., Koshimoto, Naoki, Bennett, David P., Sumi, Takahiro, Rattenbury, Nicholas J., Suzuki, Daisuke, Miyazaki, Shota, Bond, Ian A., Udalski, Andrzej, Gould, Andrew, Bozza, Valerio, Dominik, Martin, Hirao, Yuki, Kondo, Iona, Kirikawa, Rintaro, Hamada, Ryusei, Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Fujita, Katsuki, Ikeno, Tomoya, Silva, Stela Ishitani, Itow, Yoshitaka, Matsubara, Yutaka, Matsumoto, Sho, Muraki, Yasushi, Niwa, Kosuke, Okamura, Arisa, Olmschenk, Greg, Ranc, Clément, Toda, Taiga, Tomoyoshi, Mio, Tristram, Paul J., Vandorou, Aikaterini, Yama, Hibiki, Yamashita, Kansuke, Mróz, Przemek, Poleski, Radosław, Skowron, Jan, Szymański, Michał K., Poleski, Radek, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Albrow, Michael D., Chung, Sun-Ju, Han, Cheongho, Hwang, Kyu-Ha, Kim, Doeon, Jung, Youn Kil, Kim, Hyoun Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yang, Hongjing, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Jørgensen, Uffe G., Longa-Peña, Penélope, Sajadian, Sedighe, Skottfelt, Jesper, Snodgrass, Colin, Tregloan-Reed, Jeremy, Bach-Møller, Nanna, Burgdorf, Martin, D'Ago, Giuseppe, Haikala, Lauri, Hitchcock, James, Hundertmark, Markus, Khalouei, Elahe, Peixinho, Nuno, Rahvar, Sohrab, Southworth, John, Spyratos, Petros, Satoh, Yuki K., Koshimoto, Naoki, Bennett, David P., Sumi, Takahiro, Rattenbury, Nicholas J., Suzuki, Daisuke, Miyazaki, Shota, Bond, Ian A., Udalski, Andrzej, Gould, Andrew, Bozza, Valerio, Dominik, Martin, Hirao, Yuki, Kondo, Iona, Kirikawa, Rintaro, Hamada, Ryusei, Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Fujita, Katsuki, Ikeno, Tomoya, Silva, Stela Ishitani, Itow, Yoshitaka, Matsubara, Yutaka, Matsumoto, Sho, Muraki, Yasushi, Niwa, Kosuke, Okamura, Arisa, Olmschenk, Greg, Ranc, Clément, Toda, Taiga, Tomoyoshi, Mio, Tristram, Paul J., Vandorou, Aikaterini, Yama, Hibiki, Yamashita, Kansuke, Mróz, Przemek, Poleski, Radosław, Skowron, Jan, Szymański, Michał K., Poleski, Radek, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Albrow, Michael D., Chung, Sun-Ju, Han, Cheongho, Hwang, Kyu-Ha, Kim, Doeon, Jung, Youn Kil, Kim, Hyoun Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yang, Hongjing, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Jørgensen, Uffe G., Longa-Peña, Penélope, Sajadian, Sedighe, Skottfelt, Jesper, Snodgrass, Colin, Tregloan-Reed, Jeremy, Bach-Møller, Nanna, Burgdorf, Martin, D'Ago, Giuseppe, Haikala, Lauri, Hitchcock, James, Hundertmark, Markus, Khalouei, Elahe, Peixinho, Nuno, Rahvar, Sohrab, Southworth, John, and Spyratos, Petros
Abstract: We present an analysis of microlensing event OGLE-2019-BLG-0825. This event was identified as a planetary candidate by preliminary modeling. We find that significant residuals from the best-fit static binary-lens model exist and a xallarap effect can fit the residuals very well and significantly improves $\chi^2$ values. On the other hand, by including the xallarap effect in our models, we find that binary-lens parameters like mass-ratio, $q$, and separation, $s$, cannot be constrained well. However, we also find that the parameters for the source system like the orbital period and semi major axis are consistent between all the models we analyzed. We therefore constrain the properties of the source system better than the properties of the lens system. The source system comprises a G-type main-sequence star orbited by a brown dwarf with a period of $P\sim5$ days. This analysis is the first to demonstrate that the xallarap effect does affect binary-lens parameters in planetary events. It would not be common for the presence or absence of the xallarap effect to affect lens parameters in events with long orbital periods of the source system or events with transits to caustics, but in other cases, such as this event, the xallarap effect can affect binary-lens parameters., Comment: 19 pages, 7 figures, 6 tables. Accepted by AJ
Published: 2023

8. Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-Field Planets

Author: Shin, In-Gu, Yee, Jennifer C., Zang, Weicheng, Yang, Hongjing, Hwang, Kyu-Ha, Han, Cheongho, Gould, Andrew, Udalski, Andrzej, Bond, Ian A., Albrow, Michael D., Chung, Sun-Ju, Jung, Youn Kil, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Hamada, Ryusei, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Kirikawa, Rintaro, Kondo, Iona, Koshimoto, Naoki, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Olmschenk, Greg, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Sumi, Takahiro, Suzuki, Daisuke, Tomoyoshi, Mio, Tristram, Paul J., Vandorou, Aikaterini, Yama, Hibiki, Yamashita, Kansuke, Shin, In-Gu, Yee, Jennifer C., Zang, Weicheng, Yang, Hongjing, Hwang, Kyu-Ha, Han, Cheongho, Gould, Andrew, Udalski, Andrzej, Bond, Ian A., Albrow, Michael D., Chung, Sun-Ju, Jung, Youn Kil, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Hamada, Ryusei, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Kirikawa, Rintaro, Kondo, Iona, Koshimoto, Naoki, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Olmschenk, Greg, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Sumi, Takahiro, Suzuki, Daisuke, Tomoyoshi, Mio, Tristram, Paul J., Vandorou, Aikaterini, Yama, Hibiki, and Yamashita, Kansuke
Abstract: As a part of the ``Systematic KMTNet Planetary Anomaly Search" series, we report five new planets (namely, OGLE-2016-BLG-1635Lb, MOA-2016-BLG-532Lb, KMT-2016-BLG-0625Lb, OGLE-2016-BLG-1850Lb, and KMT-2016-BLG-1751Lb) and one planet candidate (KMT-2016-BLG-1855), which were found by searching $2016$ KMTNet prime fields. These $buried$ planets show a wide range of masses from Earth--class to Super--Jupiter--class, and are located in both the disk and the bulge. The ultimate goal of this series is to build a complete planet sample. Because our work provides a complementary sample to other planet detection methods, which have different detection sensitivities, our complete sample will help us to obtain a better understanding of planet demographics in our Galaxy., Comment: 38 pages, 17 figures, 12 Tables, submitted to the AAS journal
Published: 2023

9. OGLE-2017-BLG-0448Lb: A Low Mass-Ratio Wide-Orbit Microlensing Planet?

Author: Zhai, Ruocheng, Poleski, Radosław, Zang, Weicheng, Jung, Youn Kil, Udalski, Andrzej, Kuang, Renkun, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Han, Cheongho, Hwang, Kyu-Ha, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yang, Hongjing, Yee, Jennifer C., Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Ulaczyk, Krzysztof, Pietrukowicz, Paweł, Kozłowski, Szymon, Mróz, Przemek, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Wang, Hanyue, Mao, Shude, Zhang, Jiyuan, Qian, Qiyue, Zhu, Wei, Zhai, Ruocheng, Poleski, Radosław, Zang, Weicheng, Jung, Youn Kil, Udalski, Andrzej, Kuang, Renkun, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Han, Cheongho, Hwang, Kyu-Ha, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yang, Hongjing, Yee, Jennifer C., Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Ulaczyk, Krzysztof, Pietrukowicz, Paweł, Kozłowski, Szymon, Mróz, Przemek, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Wang, Hanyue, Mao, Shude, Zhang, Jiyuan, Qian, Qiyue, and Zhu, Wei
Abstract: The gravitational microlensing technique is most sensitive to planets in a Jupiter-like orbit and has detected more than 200 planets. However, only a few wide-orbit ($s > 2$) microlensing planets have been discovered, where $s$ is the planet-to-host separation normalized to the angular Einstein ring radius, $\theta_{\rm E}$. Here we present the discovery and analysis of a strong candidate wide-orbit microlensing planet in the event, OGLE-2017-BLG-0448. The whole light curve exhibits long-term residuals to the static binary-lens single-source model, so we investigate the residuals by adding the microlensing parallax, microlensing xallarap, an additional lens, or an additional source. For the first time, we observe a complex degeneracy between all four effects. The wide-orbit models with $s \sim 2.5$ and a planet-to-host mass-ratio of $q \sim 10^{-4}$ are significantly preferred, but we cannot rule out the close models with $s \sim 0.35$ and $q \sim 10^{-3}$. A Bayesian analysis based on a Galactic model indicates that, despite the complicated degeneracy, the surviving wide-orbit models all contain a super-Earth-mass to Neptune-mass planet at a projected planet-host separation of $\sim 6$ au and the surviving close-orbit models all consist of a Jovian-mass planet at $\sim 1$ au. The host star is probably an M or K dwarf. We discuss the implications of this dimension-degeneracy disaster on microlensing light-curve analysis and its potential impact on statistical studies., Comment: submitted to AJ
Published: 2023

10. OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting either a Late-Type Star or a Stellar Remnant

Author: Kirikawa, Rintaro, Sumi, Takahiro, Bennett, David P., Suzuki, Daisuke, Koshimoto, Naoki, Miyazaki, Shota, Bond, Ian A., Udalski, Andrzej, Rattenbury, Nicholas J., Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Hamada, Ryusei, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Matsubara, Yutaka, Muraki, Yasushi, Olmschenk, Greg, Ranc, Clément, Satoh, Yuki K., Tomoyoshi, Mio, Tristram, Paul . J., Vandorou, Aikaterini, Yama, Hibiki, Yamashita, Kansuke, Mróz, Przemek, Poleski, Radosław, Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Kirikawa, Rintaro, Sumi, Takahiro, Bennett, David P., Suzuki, Daisuke, Koshimoto, Naoki, Miyazaki, Shota, Bond, Ian A., Udalski, Andrzej, Rattenbury, Nicholas J., Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Hamada, Ryusei, Hirao, Yuki, Silva, Stela Ishitani, Itow, Yoshitaka, Matsubara, Yutaka, Muraki, Yasushi, Olmschenk, Greg, Ranc, Clément, Satoh, Yuki K., Tomoyoshi, Mio, Tristram, Paul . J., Vandorou, Aikaterini, Yama, Hibiki, Yamashita, Kansuke, Mróz, Przemek, Poleski, Radosław, Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, and Ulaczyk, Krzysztof
Abstract: We present the analysis of microlensing event OGLE-2014-BLG-0221, a planetary candidate event discovered in 2014. The photometric light curve is best described by a binary-lens single-source model. Our light curve modeling finds two degenerate models, with event timescales of $t_\mathrm{E}\sim70$ days and $\sim110$ days. These timescales are relatively long, indicating that the discovered system would possess a substantial mass. The two models are similar in their planetary parameters with a Jupiter mass ratio of $q \sim 10^{-3}$ and a separation of $s \sim 1.1$. While the shorter timescale model shows marginal detection of a microlensing parallax signal, the longer timescale model requires a higher order effect of microlensing parallax, lens orbital motion or xallarap to explain the deviation in the light curve. However, the modeling shows significant correlation between the higher order effects and suffers the ecliptic degeneracy that results in a failure to determine the parallax parameters. Bayesian inference is used to estimate the physical parameters of the lens, revealing the lens to be either a late-type star supported by the shorter timescale model or a stellar remnant supported by the longer timescale model. If the lens is a remnant, this would be the second planet found by microlensing around a stellar remnant. Since the models predict different values for relative proper motion and source flux, future high angular resolution follow-up observations (e.g. Keck adaptive optics) are required to rule out either of the models., Comment: 15 pages, 11 figures. Submitted to the AAS journals
Published: 2023

11. The OGLE Collection of Variable Stars. Nearly 66,000 Mira stars in the Milky Way

Author: Iwanek, Patryk, Soszyński, Igor, Kozłowski, Szymon, Poleski, Radosław, Pietrukowicz, Paweł, Skowron, Jan, Wrona, Marcin, Mróz, Przemysław, Udalski, Andrzej, Szymański, Michał K., Skowron, Dorota M., Ulaczyk, Krzysztof, Gromadzki, Mariusz, Rybicki, Krzysztof, Ratajczak, Milena, Iwanek, Patryk, Soszyński, Igor, Kozłowski, Szymon, Poleski, Radosław, Pietrukowicz, Paweł, Skowron, Jan, Wrona, Marcin, Mróz, Przemysław, Udalski, Andrzej, Szymański, Michał K., Skowron, Dorota M., Ulaczyk, Krzysztof, Gromadzki, Mariusz, Rybicki, Krzysztof, and Ratajczak, Milena
Abstract: We present a collection of 65,981 Mira-type variable stars found in the Optical Gravitational Lensing Experiment (OGLE) project database. Two-thirds of our sample (40,356 objects) are located in the Galactic bulge fields, whereas 25,625 stars are in the Galactic disk. The vast majority of the collection (47,532 objects) are new discoveries. We provide basic observational parameters of the Mira variables: equatorial coordinates, pulsation periods, $I$-band and $V$-band mean magnitudes, $I$-band brightness amplitudes, and identifications in other catalogs of variable stars. We also provide the $I$-band and $V$-band time-series photometry collected since 1997 during the OGLE-II, OGLE-III, and OGLE-IV phases. The classical selection process, i.e., mostly based on the visual inspection of light curves by experienced astronomers, led us to the high purity of the catalog. As a result, this collection can be used as a training set in the machine learning classification algorithms. Using overlapping parts of adjacent OGLE fields, we estimate the completeness of the catalog to be about 96%. We compare and discuss the statistical features of Miras located in different regions of the Milky Way. We show examples of stars that change their type over time, from a semi-regular variable to Mira and vice versa. This dataset is perfectly suited to study the three-dimensional structure of the Milky Way, and it may help to explain the puzzle of the X-shaped bulge., Comment: Accepted for publication in The Astrophysical Journal Supplement Series. 18 pages, 8 figures, 3 tables. The OGLE Collection of Miras in the Milky Way is publicly available through http://www.astrouw.edu.pl/ogle/ogle4/OCVS/blg/lpv/ for Miras located in the Galactic bulge fields, and http://www.astrouw.edu.pl/ogle/ogle4/OCVS/gd/lpv/ for Miras located in the Galactic disk fields
Published: 2022

12. OGLE-2018-BLG-0584 and KMT-2018-BLG-2119: two microlensing events with two lens masses and two source stars

Author: Han, Cheongho, Udalski, Andrzej, Jung, Youn Kil, Kim, Doeon, Yang, Hongjing, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Kim, Hyoun-Woo, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Udalski, Andrzej, Jung, Youn Kil, Kim, Doeon, Yang, Hongjing, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Kim, Hyoun-Woo, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shvartzvald, Yossi, Shin, In-Gu, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We conduct a systematic investigation of the microlensing data collected during the previous observation seasons for the purpose of reanalyzing anomalous lensing events with no suggested plausible models. We find that two anomalous lensing events OGLE-2018-BLG-0584 and KMT-2018-BLG-2119 cannot be explained with the usual models based on either a binary-lens single-source (2L1S) or a single-lens binary-source (1L2S) interpretation. We test the feasibility of explaining the light curves with more sophisticated models by adding an extra lens (3L1S model) or a source (2L2S model) component to the 2L1S lens-system configuration. We find that a 2L2S interpretation well explains the light curves of both events, for each of which there are a pair of solutions resulting from the close and wide degeneracy. For the event OGLE-2018-BLG-0584, the source is a binary composed of two K-type stars, and the lens is a binary composed of two M dwarfs. For KMT-2018-BLG-2119, the source is a binary composed of two dwarfs of G and K spectral types, and the lens is a binary composed of a low-mass M dwarf and a brown dwarf., Comment: 9 pages, 9 figures
Published: 2022
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13. A three-dimensional map of the Milky Way using 66,000 Mira variable stars

Author: Iwanek, Patryk, Poleski, Radosław, Kozłowski, Szymon, Soszyński, Igor, Pietrukowicz, Paweł, Ban, Makiko, Skowron, Jan, Mróz, Przemysław, Wrona, Marcin, Udalski, Andrzej, Szymański, Michał K., Skowron, Dorota M., Ulaczyk, Krzysztof, Gromadzki, Mariusz, Rybicki, Krzysztof, Ratajczak, Milena, Iwanek, Patryk, Poleski, Radosław, Kozłowski, Szymon, Soszyński, Igor, Pietrukowicz, Paweł, Ban, Makiko, Skowron, Jan, Mróz, Przemysław, Wrona, Marcin, Udalski, Andrzej, Szymański, Michał K., Skowron, Dorota M., Ulaczyk, Krzysztof, Gromadzki, Mariusz, Rybicki, Krzysztof, and Ratajczak, Milena
Abstract: We study the three-dimensional structure of the Milky Way using 65,981 Mira variable stars discovered by the Optical Gravitational Lensing Experiment (OGLE) survey. The spatial distribution of the Mira stars is analyzed with a model containing three barred components that include the X-shaped boxy component in the Galactic center (GC), and an axisymmetric disk. We take into account the distance uncertainties by implementing the Bayesian hierarchical inference method. The distance to the GC is $R_0 = 7.66 \pm 0.01 \mathrm{(stat.)} \pm 0.39 \mathrm{(sys.)}$ kpc, while the inclination of the major axis of the bulge to the Sun-GC line-of-sight is $\theta = 20.2^\circ \pm 0.6^\circ \mathrm{(stat.)} \pm 0.7^\circ \mathrm{(sys.)} $. We present, for the first time, a detailed three-dimensional map of the Milky Way composed of young and intermediate-age stellar populations. Our analysis provides independent evidence for both the X-shaped bulge component and the flaring disk (being plausibly warped). We provide the complete dataset of properties of Miras that were used for calculations in this work. The table includes: mean brightness and amplitudes in nine photometric bands (covering a range of wavelength from 0.5 to 12 $\mu$m), photometric chemical type, estimated extinction, and calculated distance with its uncertainty for each Mira variable. The median distance accuracy to a Mira star is at the level of $6.6\%$., Comment: Accepted for publication in The Astrophysical Journal Supplement Series. 22 pages, 7 figures, 2 tables. The full machine readable Table 1 and corner plot are available through the OGLE website via https://www.astrouw.edu.pl/ogle/ogle4/MILKY_WAY_3D_MAP/, and Zenodo via https://doi.org/10.5281/zenodo.7472598
Published: 2022
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14. An X-ray quiet black hole born with a negligible kick in a massive binary within the Large Magellanic Cloud

Author: Shenar, Tomer, Sana, Hugues, Mahy, Laurent, El-Badry, Kareem, Marchant, Pablo, Langer, Norbert, Hawcroft, Calum, Fabry, Matthias, Sen, Koushik, Almeida, Leonardo A., Abdul-Masih, Michael, Bodensteiner, Julia, Crowther, Paul A., Gieles, Mark, Gromadzki, Mariusz, Henault-Brunet, Vincent, Herrero, Artemio, de Koter, Alex, Iwanek, Patryk, Kozłowski, Szymon, Lennon, Daniel J., Apellaniz, Jesus Maız, Mroz, Przemysław, Moffat, Anthony F. J., Picco, Annachiara, Pietrukowicz, Paweł, Poleski, Radosław, Rybicki, Krzysztof, Schneider, Fabian R. N., Skowron, Dorota M., Skowron, Jan, Soszynski, Igor, Szymanski, Michał K., Toonen, Silvia, Udalski, Andrzej, Ulaczyk, Krzysztof, Vink, Jorick S., Wrona, Marcin, Shenar, Tomer, Sana, Hugues, Mahy, Laurent, El-Badry, Kareem, Marchant, Pablo, Langer, Norbert, Hawcroft, Calum, Fabry, Matthias, Sen, Koushik, Almeida, Leonardo A., Abdul-Masih, Michael, Bodensteiner, Julia, Crowther, Paul A., Gieles, Mark, Gromadzki, Mariusz, Henault-Brunet, Vincent, Herrero, Artemio, de Koter, Alex, Iwanek, Patryk, Kozłowski, Szymon, Lennon, Daniel J., Apellaniz, Jesus Maız, Mroz, Przemysław, Moffat, Anthony F. J., Picco, Annachiara, Pietrukowicz, Paweł, Poleski, Radosław, Rybicki, Krzysztof, Schneider, Fabian R. N., Skowron, Dorota M., Skowron, Jan, Soszynski, Igor, Szymanski, Michał K., Toonen, Silvia, Udalski, Andrzej, Ulaczyk, Krzysztof, Vink, Jorick S., and Wrona, Marcin
Abstract: Stellar-mass black holes are the final remnants of stars born with more than 15 solar masses. Billions are expected to reside in the Local Group, yet only few are known, mostly detected through X-rays emitted as they accrete material from a companion star. Here, we report on VFTS 243: a massive X-ray faint binary in the Large Magellanic Cloud. With an orbital period of 10.4-d, it comprises an O-type star of 25 solar masses and an unseen companion of at least nine solar masses. Our spectral analysis excludes a non-degenerate companion at a 5-sigma confidence level. The minimum companion mass implies that it is a black hole. No other X-ray quiet black hole is unambiguously known outside our Galaxy. The (near-)circular orbit and kinematics of VFTS 243 imply that the collapse of the progenitor into a black hole was associated with little or no ejected material or black-hole kick. Identifying such unique binaries substantially impacts the predicted rates of gravitational-wave detections and properties of core-collapse supernovae across the Cosmos., Comment: Accepted to Nature Astronomy, 64 pages, 15 figures, 2 tables; ESO press release: https://www.eso.org/public/news/eso2210/; Nat Asr paper URL: https://www.nature.com/articles/s41550-022-01730-y
Published: 2022
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15. Four sub-Jovian-mass planets detected by high-cadence microlensing surveys

Author: Han, Cheongho, Kim, Doeon, Gould, Andrew, Udalski, Andrzej, Bond, Ian A., Bozza, Valerio, Jung, Youn Kil, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Abe, Fumio, Barry, Richard K., Bennett, David P., Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kirikawa, Rintaro, Koshimoto, Naoki, Kondo, Iona, Matsubara, Yutaka, Matsumoto, Sho, Miyazaki, Shota, Muraki, Yasushi, Olmschenk, Greg, Okamura, Arisa, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Silva, Stela Ishitani, Sumi, Takahiro, Suzuki, Daisuke, Toda, Taiga, Tristram, Paul J., Vandorou, Aikaterini, Yama, Hibiki, Han, Cheongho, Kim, Doeon, Gould, Andrew, Udalski, Andrzej, Bond, Ian A., Bozza, Valerio, Jung, Youn Kil, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Abe, Fumio, Barry, Richard K., Bennett, David P., Bhattacharya, Aparna, Fujii, Hirosane, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kirikawa, Rintaro, Koshimoto, Naoki, Kondo, Iona, Matsubara, Yutaka, Matsumoto, Sho, Miyazaki, Shota, Muraki, Yasushi, Olmschenk, Greg, Okamura, Arisa, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Silva, Stela Ishitani, Sumi, Takahiro, Suzuki, Daisuke, Toda, Taiga, Tristram, Paul J., Vandorou, Aikaterini, and Yama, Hibiki
Abstract: With the aim of finding short-term planetary signals, we investigated the data collected from the high-cadence microlensing surveys. From this investigation, we found four planetary systems with low planet-to-host mass ratios, including OGLE-2017-BLG-1691L, KMT-2021-BLG-0320L, KMT-2021-BLG-1303L, and KMT-2021-BLG-1554L. Despite the short durations, ranging from a few hours to a couple of days, the planetary signals were clearly detected by the combined data of the lensing surveys. It is found that three of the planetary systems have mass ratios of the order of $10^{-4}$ and the other has a mass ratio slightly greater than $10^{-3}$. The estimated masses indicate that all discovered planets have sub-Jovian masses. The planet masses of KMT-2021-BLG-0320Lb, KMT-2021-BLG-1303Lb, and KMT-2021-BLG-1554Lb correspond to $\sim 0.10$, $\sim 0.38$, and $\sim 0.12$ times of the mass of the Jupiter, and the mass of OGLE-2017-BLG-1691Lb corresponds to that of the Uranus. The estimated mass of the planet host KMT-2021-BLG-1554L, $M_{\rm host}\sim 0.08~M_\odot$, corresponds to the boundary between a star and a brown dwarf. Besides this system, the host stars of the other planetary systems are low-mass stars with masses in the range of $\sim [0.3$--$0.6]~M_\odot$. The discoveries of the planets well demonstrate the capability of the current high-cadence microlensing surveys in detecting low-mass planets., Comment: 12 pages, 12 figures, 9 tables
Published: 2022
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16. The OGLE Collection of Variable Stars. Nearly 66,000 Mira stars in the Milky Way

Author: Iwanek, Patryk, Soszyński, Igor, Kozłowski, Szymon, Poleski, Radosław, Pietrukowicz, Paweł, Skowron, Jan, Wrona, Marcin, Mróz, Przemysław, Udalski, Andrzej, Szymański, Michał K., Skowron, Dorota M., Ulaczyk, Krzysztof, Gromadzki, Mariusz, Rybicki, Krzysztof, Ratajczak, Milena, Iwanek, Patryk, Soszyński, Igor, Kozłowski, Szymon, Poleski, Radosław, Pietrukowicz, Paweł, Skowron, Jan, Wrona, Marcin, Mróz, Przemysław, Udalski, Andrzej, Szymański, Michał K., Skowron, Dorota M., Ulaczyk, Krzysztof, Gromadzki, Mariusz, Rybicki, Krzysztof, and Ratajczak, Milena
Abstract: We present a collection of 65,981 Mira-type variable stars found in the Optical Gravitational Lensing Experiment (OGLE) project database. Two-thirds of our sample (40,356 objects) are located in the Galactic bulge fields, whereas 25,625 stars are in the Galactic disk. The vast majority of the collection (47,532 objects) are new discoveries. We provide basic observational parameters of the Mira variables: equatorial coordinates, pulsation periods, $I$-band and $V$-band mean magnitudes, $I$-band brightness amplitudes, and identifications in other catalogs of variable stars. We also provide the $I$-band and $V$-band time-series photometry collected since 1997 during the OGLE-II, OGLE-III, and OGLE-IV phases. The classical selection process, i.e., mostly based on the visual inspection of light curves by experienced astronomers, led us to the high purity of the catalog. As a result, this collection can be used as a training set in the machine learning classification algorithms. Using overlapping parts of adjacent OGLE fields, we estimate the completeness of the catalog to be about 96%. We compare and discuss the statistical features of Miras located in different regions of the Milky Way. We show examples of stars that change their type over time, from a semi-regular variable to Mira and vice versa. This dataset is perfectly suited to study the three-dimensional structure of the Milky Way, and it may help to explain the puzzle of the X-shaped bulge., Comment: Accepted for publication in The Astrophysical Journal Supplement Series. 18 pages, 8 figures, 3 tables. The OGLE Collection of Miras in the Milky Way is publicly available through http://www.astrouw.edu.pl/ogle/ogle4/OCVS/blg/lpv/ for Miras located in the Galactic bulge fields, and http://www.astrouw.edu.pl/ogle/ogle4/OCVS/gd/lpv/ for Miras located in the Galactic disk fields
Published: 2022
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17. OGLE-2019-BLG-0468Lb,c: two microlensing giant planets around a G-type star

Author: Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Buckley, David, Dong, Subo, Luo, Ali, Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Buckley, David, Dong, Subo, and Luo, Ali
Abstract: With the aim of interpreting anomalous lensing events with no suggested models, we conducted a project of reinvestigating microlensing data in and before the 2019 season. In this work, we report a multi-planet system OGLE-2019-BLG-0468L found from the project. The light curve of the lensing event OGLE-2019-BLG-0468, which consists of three distinctive anomaly features, could not be explained by the usual binary-lens or binary-source interpretation. We find a solution explaining all anomaly features with a triple-lens interpretation, in which the lens is composed of two planets and their host, making the lens the fourth multi-planet system securely found by microlensing. The two planets have masses $\sim 3.4~M_{\rm J}$ and $\sim 10.2~M_{\rm J}$, and they are orbiting around a G-type star with a mass $\sim 0.9~M_\odot$ and a distance $\sim 4.4$ kpc. The host of the planets is most likely responsible for the light of the baseline object, although the possibility for the host to be a companion to the baseline object cannot be ruled out., Comment: 10 pages, 3 tables, 11 figures
Published: 2021
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18. The OGLE Collection of Variable Stars. One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds

Author: Wrona, Marcin, Ratajczak, Milena, Kołaczek-Szymański, Piotr A., Kozłowski, Szymon, Soszyński, Igor, Iwanek, Patryk, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Skowron, Dorota M., Skowron, Jan, Mróz, Przemysław, Poleski, Radosław, Gromadzki, Mariusz, Ulaczyk, Krzysztof, Rybicki, Krzysztof, Wrona, Marcin, Ratajczak, Milena, Kołaczek-Szymański, Piotr A., Kozłowski, Szymon, Soszyński, Igor, Iwanek, Patryk, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Skowron, Dorota M., Skowron, Jan, Mróz, Przemysław, Poleski, Radosław, Gromadzki, Mariusz, Ulaczyk, Krzysztof, and Rybicki, Krzysztof
Abstract: We present a collection of 991 heartbeat star (HBS) candidates found in the Optical Gravitational Lensing Experiment (OGLE) project data archive. We discuss the selection process of the HBS candidates and the structure of the catalog itself. It consists of 512 stars located toward the Galactic bulge (GB), 439 stars located in the Large Magellanic Cloud (LMC), and 40 in the Small Magellanic Cloud (SMC). The collection contains two large groups of HBSs with different physical properties. The main distinction between the two groups is the evolutionary status of the primary star. The first group of about 100 systems contains a hot main-sequence (MS) or a Hertzsprung-gap primary star, while the second group of about 900 systems includes a red giant (RG). For each star, we provide two-decade-long time-series photometry, in the Cousins $I$- and Johnson $V$-band filters, obtained by the OGLE project. We also present basic observational information as well as orbital parameters derived from the light curve modeling., Comment: 13 pages (17 pages in arXiv version), 11 figures, 5 tables. The full machine-readable tables are provided by the publisher. The catalog is available via OGLE website: https://astrouw.edu.pl/ogle/ogle4/OCVS/. Erratum; in the publisher version of the paper, there are wrong reference numbers to the figures from Paper II: Figures 8--9 --> Figures 9--10, Figure 10 --> Figure 11, Figure 11 --> Figure 12
Published: 2021
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19. OGLE-2019-BLG-0304: Competing Interpretations between a Planet-binary Model and a Binary-source + Binary-lens model

Author: Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Ryu, Yoon-Hyun, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Ryu, Yoon-Hyun, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We analyze the microlensing event OGLE-2019-BLG-0304, whose light curve exhibits two distinctive features: a deviation in the peak region and a second bump appearing $\sim 61$~days after the main peak. Although a binary-lens model can explain the overall features, it leaves subtle but noticeable residuals in the peak region. We find that the residuals can be explained by the presence of either a planetary companion located close to the primary of the binary lens (3L1S model) or an additional close companion to the source (2L2S model). Although the 3L1S model is favored over the 2L2S model, with $\Delta\chi^2\sim 8$, securely resolving the degeneracy between the two models is difficult with the currently available photometric data. According to the 3L1S interpretation, the lens is a planetary system, in which a planet with a mass $0.51^{+0.51}_{-0.23}~M_{\rm J}$ is in an S-type orbit around a binary composed of stars with masses $0.27^{+0.27}_{-0.12}~M_\odot$ and $0.10^{+0.10}_{-0.04}~M_\odot$. According to the 2L2S interpretation, on the other hand, the source is composed of G- and K-type giant stars, and the lens is composed of a low-mass M dwarf and a brown dwarf with masses $0.12^{+0.12}_{-0.05}~M_\odot$ and $0.045^{+0.045}_{-.019}~M_\odot$, respectively. The event illustrates the need for through model testing in the interpretation of lensing events with complex features in light curves., Comment: 11 pages, 3 tables, 11 figures
Published: 2021
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20. Final Targeting Strategy for the SDSS-IV APOGEE-2S Survey

Author: Santana, Felipe A., Beaton, Rachael L., Covey, Kevin R., O'Connell, Julia E., Longa-Peña, Penélope, Cohen, Roger, Fernández-Trincado, José G., Hayes, Christian R., Zasowski, Gail, Sobeck, Jennifer S., Majewski, Steven R., Chojnowski, S. D., De Lee, Nathan, Oelkers, Ryan J., Stringfellow, Guy S., Almeida, Andrés, Anguiano, Borja, Donor, John, Frinchaboy, Peter M., Hasselquist, Sten, Johnson, Jennifer A., Kollmeier, Juna A., Nidever, David L., Price-Whelan, Adrian. M., Rojas-Arriagada, Alvaro, Schultheis, Mathias, Shetrone, Matthew, Simon, Joshua D., Aerts, Conny, Borissova, Jura, Drout, Maria R., Geisler, Doug, Law, C. Y., Medina, Nicolás, Minniti, Dante, Monachesi, Antonela, Muñoz, Ricardo R., Poleski, Radosław, Roman-Lopes, Alexandre, Schlaufman, Kevin C., Stutz, Amelia M., Teske, Johanna, Tkachenko, Andrew, Van Saders, Jennifer L., Weinberger, Alycia, Zoccali, Manuela, Santana, Felipe A., Beaton, Rachael L., Covey, Kevin R., O'Connell, Julia E., Longa-Peña, Penélope, Cohen, Roger, Fernández-Trincado, José G., Hayes, Christian R., Zasowski, Gail, Sobeck, Jennifer S., Majewski, Steven R., Chojnowski, S. D., De Lee, Nathan, Oelkers, Ryan J., Stringfellow, Guy S., Almeida, Andrés, Anguiano, Borja, Donor, John, Frinchaboy, Peter M., Hasselquist, Sten, Johnson, Jennifer A., Kollmeier, Juna A., Nidever, David L., Price-Whelan, Adrian. M., Rojas-Arriagada, Alvaro, Schultheis, Mathias, Shetrone, Matthew, Simon, Joshua D., Aerts, Conny, Borissova, Jura, Drout, Maria R., Geisler, Doug, Law, C. Y., Medina, Nicolás, Minniti, Dante, Monachesi, Antonela, Muñoz, Ricardo R., Poleski, Radosław, Roman-Lopes, Alexandre, Schlaufman, Kevin C., Stutz, Amelia M., Teske, Johanna, Tkachenko, Andrew, Van Saders, Jennifer L., Weinberger, Alycia, and Zoccali, Manuela
Abstract: APOGEE is a high-resolution (R sim 22,000), near-infrared, multi-epoch, spectroscopic survey of the Milky Way. The second generation of the APOGEE project, APOGEE-2, includes an expansion of the survey to the Southern Hemisphere called APOGEE-2S. This expansion enabled APOGEE to perform a fully panoramic mapping of all the main regions of the Milky Way; in particular, by operating in the H-band, APOGEE is uniquely able to probe the dust-hidden inner regions of the Milky Way that are best accessed from the Southern Hemisphere. In this paper we present the targeting strategy of APOGEE-2S, with special attention to documenting modifications to the original, previously published plan. The motivation for these changes is explained as well as an assessment of their effectiveness in achieving their intended scientific objective. In anticipation of this being the last paper detailing APOGEE targeting, we present an accounting of all such information complete through the end of the APOGEE-2S project; this includes several main survey programs dedicated to exploration of major stellar populations and regions of the Milky Way, as well as a full list of programs contributing to the APOGEE database through allocations of observing time by the Chilean National Time Allocation Committee (CNTAC) and the Carnegie Institution for Science (CIS). This work was presented along with a companion article, R. Beaton et al. (submitted; AAS29028), presenting the final target selection strategy adopted for APOGEE-2 in the Northern Hemisphere., Comment: 43 pages; 5 figures; 6 Tables; 1 Appendix; Submitted to Journal and Under Review; Posting to accompany papers using the SDSS-IV/APOGEE-2 Data Release 17 scheduled for December 2021
Published: 2021
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21. Three faint-source microlensing planets detected via resonant-caustic channel

Author: Han, Cheongho, Udalski, Andrzej, Kim, Doeon, Ryu, Yoon-Hyun, Bozza, Valerio, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Udalski, Andrzej, Kim, Doeon, Ryu, Yoon-Hyun, Bozza, Valerio, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We conducted a project of reinvestigating the 2017--2019 microlensing data collected by the high-cadence surveys with the aim of finding planets that were missed due to the deviations of planetary signals from the typical form of short-term anomalies. The project led us to find three planets including KMT-2017-BLG-2509Lb, OGLE-2017-BLG-1099Lb, and OGLE-2019-BLG-0299Lb. The lensing light curves of the events have a common characteristic that the planetary signals were produced by the crossings of faint source stars over the resonant caustics formed by giant planets located near the Einstein rings of host stars. For all planetary events, the lensing solutions are uniquely determined without any degeneracy. It is estimated that the host masses are in the range of $0.45\lesssim M/M_\odot \lesssim 0.59$, which corresponds to early M to late K dwarfs, and thus the host stars are less massive than the sun. On the other hand, the planets, with masses in the range of $2.1\lesssim M/M_{\rm J}\lesssim 6.2$, are heavier than the heaviest planet of the solar system, that is, Jupiter. The planets in all systems lie beyond the snow lines of the hosts, and thus the discovered planetary systems, together with many other microlensing planetary systems, support that massive gas-giant planets are commonplace around low-mass stars. We discuss the role of late-time high-resolution imaging in clarifying resonant-image lenses with very faint sources., Comment: 10 pages, 13 figures, 6 tables
Published: 2021
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22. Multiwavelength properties of Miras

Author: Iwanek, Patryk, Kozłowski, Szymon, Gromadzki, Mariusz, Soszyński, Igor, Wrona, Marcin, Skowron, Jan, Ratajczak, Milena, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Poleski, Radosław, Mróz, Przemysław, Skowron, Dorota M., Rybicki, Krzysztof, Iwanek, Patryk, Kozłowski, Szymon, Gromadzki, Mariusz, Soszyński, Igor, Wrona, Marcin, Skowron, Jan, Ratajczak, Milena, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Poleski, Radosław, Mróz, Przemysław, Skowron, Dorota M., and Rybicki, Krzysztof
Abstract: We comprehensively study the variability of Miras in the Large Magellanic Cloud (LMC) by simultaneous analysing light curves in 14 bands in the range of 0.5$-$24 microns. We model over 20-years-long, high cadence $I$-band light curves collected by The Optical Gravitational Lensing Experiment (OGLE) and fit them to light curves collected in the remaining optical/near-infrared/mid-infrared bands to derive both the variability amplitude ratio and phase-lag as a function of wavelength. We show that the variability amplitude ratio declines with the increasing wavelength for both oxygen-rich (O-rich) and carbon-rich (C-rich) Miras, while the variability phase-lag increases slightly with the increasing wavelength. In a significant number of Miras, mostly the C-rich ones, the spectral energy distributions (SEDs) require a presence of a cool component (dust) in order to match the mid-IR data. Based on SED fits for a golden sample of 140 Miras, we calculated synthetic period-luminosity relations (PLRs) in 42 bands for the existing and future sky surveys that include OGLE, The VISTA Near-Infrared $YJK_\mathrm{s}$ Survey of the Magellanic Clouds System (VMC), Legacy Survey of Space and Time (LSST), Gaia, Spitzer, The Wide-field Infrared Survey Explorer (WISE), The James Webb Space Telescope (JWST), The Nancy Grace Roman Space Telescope (formerly WFIRST), and The Hubble Space Telescope (HST). We show that the synthetic PLR slope decreases with increasing wavelength for both the O-rich and C-rich Miras in the range of 0.1$-$40 microns. Finally, we show the location and motions of Miras on the color-magnitude (CMD) and color-color (CCD) diagrams., Comment: Accepted for publication in The Astrophysical Journal Supplement Series. 27 pages, 16 figures, 7 tables. The full machine readable tables will be available in the online journal just after publication
Published: 2021
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23. Determination of rotation periods for a large sample of asteroids from K2 Campaign 9

Author: Podlewska-Gaca, Edyta, Poleski, Radosław, Bartczak, Przemysław, McDonald, Iain, Pál, András, Podlewska-Gaca, Edyta, Poleski, Radosław, Bartczak, Przemysław, McDonald, Iain, and Pál, András
Abstract: Kepler mission is a powerful tool in the study the different types of astrophysical objects or events in the distant Universe. However, the spacecraft gives also the opportunity to study Solar System objects passing in the telescope field of view. The aim of this paper is to determine for the first time the rotation periods of a number of asteroids observed by the Kepler satellite during the K2 Campaign 9. Using publicly available data from Kepler mission we have used the Modified Causal Pixel Model (MCPM) code to perform the aperture-like and PRF-like photometry of 1026 asteroids. The results allowed us to determine the rotation periods for 188 asteroids. For asteroids with rotation periods previously measured, we compared the results and found very good agreement. There are additional 20 asteroids for which we obtained lower limits on rotation periods and in all cases these limits are at least 100 h., Comment: 24 pages, 8 figures, submitted to ApJS
Published: 2021
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24. Measuring the mass function of isolated stellar remnants with gravitational microlensing. II. Analysis of the OGLE-III data

Author: Mróz, Przemek, Udalski, Andrzej, Wyrzykowski, Łukasz, Skowron, Jan, Poleski, Radosław, Szymanski, Michał K., Soszyński, Igor, Ulaczyk, Krzysztof, Mróz, Przemek, Udalski, Andrzej, Wyrzykowski, Łukasz, Skowron, Jan, Poleski, Radosław, Szymanski, Michał K., Soszyński, Igor, and Ulaczyk, Krzysztof
Abstract: Our knowledge of the birth mass function of neutron stars and black holes is based on observations of binary systems but the binary evolution likely affects the final mass of the compact object. Gravitational microlensing allows us to detect and measure masses of isolated stellar remnants, which are nearly impossible to obtain with other techniques. Here, we analyze a sample of 4360 gravitational microlensing events detected during the third phase of the OGLE survey. We select a subsample of 87 long-timescale low-blending events. We estimate the masses of lensing objects by combining photometric data from OGLE and proper-motion information from OGLE and Gaia EDR3. We find 35 high-probability dark lenses - white dwarfs, neutron stars, and black holes - which we use to constrain the mass function of isolated stellar remnants. In the range 1-100 M_⊙, occupied by neutron stars and black holes, the remnant mass function is continuous and can be approximated as a power-law with a slope of 0.83^(+0.16)_(−0.18) with a tentative evidence against a broad gap between neutron stars and black holes. This slope is slightly flatter than the slope of the mass function of black holes detected by gravitational wave detectors LIGO and Virgo, although both values are consistent with each other within the quoted error bars. The measured slope of the remnant mass function agrees with predictions of some population synthesis models of black hole formation.
Published: 2021

25. OGLE-2019-BLG-0468Lb,c: two microlensing giant planets around a G-type star

Author: Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Buckley, David, Dong, Subo, Luo, Ali, Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Rybicki, Krzysztof A., Iwanek, Patryk, Ulaczyk, Krzysztof, Wrona, Marcin, Gromadzki, Mariusz, Buckley, David, Dong, Subo, and Luo, Ali
Abstract: With the aim of interpreting anomalous lensing events with no suggested models, we conducted a project of reinvestigating microlensing data in and before the 2019 season. In this work, we report a multi-planet system OGLE-2019-BLG-0468L found from the project. The light curve of the lensing event OGLE-2019-BLG-0468, which consists of three distinctive anomaly features, could not be explained by the usual binary-lens or binary-source interpretation. We find a solution explaining all anomaly features with a triple-lens interpretation, in which the lens is composed of two planets and their host, making the lens the fourth multi-planet system securely found by microlensing. The two planets have masses $\sim 3.4~M_{\rm J}$ and $\sim 10.2~M_{\rm J}$, and they are orbiting around a G-type star with a mass $\sim 0.9~M_\odot$ and a distance $\sim 4.4$ kpc. The host of the planets is most likely responsible for the light of the baseline object, although the possibility for the host to be a companion to the baseline object cannot be ruled out., Comment: 10 pages, 3 tables, 11 figures
Published: 2021
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26. The OGLE Collection of Variable Stars. One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds

Author: Wrona, Marcin, Ratajczak, Milena, Kołaczek-Szymański, Piotr A., Kozłowski, Szymon, Soszyński, Igor, Iwanek, Patryk, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Skowron, Dorota M., Skowron, Jan, Mróz, Przemysław, Poleski, Radosław, Gromadzki, Mariusz, Ulaczyk, Krzysztof, Rybicki, Krzysztof, Wrona, Marcin, Ratajczak, Milena, Kołaczek-Szymański, Piotr A., Kozłowski, Szymon, Soszyński, Igor, Iwanek, Patryk, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Skowron, Dorota M., Skowron, Jan, Mróz, Przemysław, Poleski, Radosław, Gromadzki, Mariusz, Ulaczyk, Krzysztof, and Rybicki, Krzysztof
Abstract: We present a collection of 991 heartbeat star (HBS) candidates found in the Optical Gravitational Lensing Experiment (OGLE) project data archive. We discuss the selection process of the HBS candidates and the structure of the catalog itself. It consists of 512 stars located toward the Galactic bulge (GB), 439 stars located in the Large Magellanic Cloud (LMC), and 40 in the Small Magellanic Cloud (SMC). The collection contains two large groups of HBSs with different physical properties. The main distinction between the two groups is the evolutionary status of the primary star. The first group of about 100 systems contains a hot main-sequence (MS) or a Hertzsprung-gap primary star, while the second group of about 900 systems includes a red giant (RG). For each star, we provide two-decade-long time-series photometry, in the Cousins $I$- and Johnson $V$-band filters, obtained by the OGLE project. We also present basic observational information as well as orbital parameters derived from the light curve modeling., Comment: 13 pages (17 pages in arXiv version), 11 figures, 5 tables. The full machine-readable tables are provided by the publisher. The catalog is available via OGLE website: https://astrouw.edu.pl/ogle/ogle4/OCVS/. Erratum; in the publisher version of the paper, there are wrong reference numbers to the figures from Paper II: Figures 8--9 --> Figures 9--10, Figure 10 --> Figure 11, Figure 11 --> Figure 12
Published: 2021
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27. OGLE-2019-BLG-0304: Competing Interpretations between a Planet-binary Model and a Binary-source + Binary-lens model

Author: Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Ryu, Yoon-Hyun, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Kim, Doeon, Ryu, Yoon-Hyun, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Hyoun-Woo, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We analyze the microlensing event OGLE-2019-BLG-0304, whose light curve exhibits two distinctive features: a deviation in the peak region and a second bump appearing $\sim 61$~days after the main peak. Although a binary-lens model can explain the overall features, it leaves subtle but noticeable residuals in the peak region. We find that the residuals can be explained by the presence of either a planetary companion located close to the primary of the binary lens (3L1S model) or an additional close companion to the source (2L2S model). Although the 3L1S model is favored over the 2L2S model, with $\Delta\chi^2\sim 8$, securely resolving the degeneracy between the two models is difficult with the currently available photometric data. According to the 3L1S interpretation, the lens is a planetary system, in which a planet with a mass $0.51^{+0.51}_{-0.23}~M_{\rm J}$ is in an S-type orbit around a binary composed of stars with masses $0.27^{+0.27}_{-0.12}~M_\odot$ and $0.10^{+0.10}_{-0.04}~M_\odot$. According to the 2L2S interpretation, on the other hand, the source is composed of G- and K-type giant stars, and the lens is composed of a low-mass M dwarf and a brown dwarf with masses $0.12^{+0.12}_{-0.05}~M_\odot$ and $0.045^{+0.045}_{-.019}~M_\odot$, respectively. The event illustrates the need for through model testing in the interpretation of lensing events with complex features in light curves., Comment: 11 pages, 3 tables, 11 figures
Published: 2021
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28. Three faint-source microlensing planets detected via resonant-caustic channel

Author: Han, Cheongho, Udalski, Andrzej, Kim, Doeon, Ryu, Yoon-Hyun, Bozza, Valerio, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Udalski, Andrzej, Kim, Doeon, Ryu, Yoon-Hyun, Bozza, Valerio, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We conducted a project of reinvestigating the 2017--2019 microlensing data collected by the high-cadence surveys with the aim of finding planets that were missed due to the deviations of planetary signals from the typical form of short-term anomalies. The project led us to find three planets including KMT-2017-BLG-2509Lb, OGLE-2017-BLG-1099Lb, and OGLE-2019-BLG-0299Lb. The lensing light curves of the events have a common characteristic that the planetary signals were produced by the crossings of faint source stars over the resonant caustics formed by giant planets located near the Einstein rings of host stars. For all planetary events, the lensing solutions are uniquely determined without any degeneracy. It is estimated that the host masses are in the range of $0.45\lesssim M/M_\odot \lesssim 0.59$, which corresponds to early M to late K dwarfs, and thus the host stars are less massive than the sun. On the other hand, the planets, with masses in the range of $2.1\lesssim M/M_{\rm J}\lesssim 6.2$, are heavier than the heaviest planet of the solar system, that is, Jupiter. The planets in all systems lie beyond the snow lines of the hosts, and thus the discovered planetary systems, together with many other microlensing planetary systems, support that massive gas-giant planets are commonplace around low-mass stars. We discuss the role of late-time high-resolution imaging in clarifying resonant-image lenses with very faint sources., Comment: 10 pages, 13 figures, 6 tables
Published: 2021
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29. Final Targeting Strategy for the SDSS-IV APOGEE-2S Survey

Author: Santana, Felipe A., Beaton, Rachael L., Covey, Kevin R., O'Connell, Julia E., Longa-Peña, Penélope, Cohen, Roger, Fernández-Trincado, José G., Hayes, Christian R., Zasowski, Gail, Sobeck, Jennifer S., Majewski, Steven R., Chojnowski, S. D., De Lee, Nathan, Oelkers, Ryan J., Stringfellow, Guy S., Almeida, Andrés, Anguiano, Borja, Donor, John, Frinchaboy, Peter M., Hasselquist, Sten, Johnson, Jennifer A., Kollmeier, Juna A., Nidever, David L., Price-Whelan, Adrian. M., Rojas-Arriagada, Alvaro, Schultheis, Mathias, Shetrone, Matthew, Simon, Joshua D., Aerts, Conny, Borissova, Jura, Drout, Maria R., Geisler, Doug, Law, C. Y., Medina, Nicolás, Minniti, Dante, Monachesi, Antonela, Muñoz, Ricardo R., Poleski, Radosław, Roman-Lopes, Alexandre, Schlaufman, Kevin C., Stutz, Amelia M., Teske, Johanna, Tkachenko, Andrew, Van Saders, Jennifer L., Weinberger, Alycia, Zoccali, Manuela, Santana, Felipe A., Beaton, Rachael L., Covey, Kevin R., O'Connell, Julia E., Longa-Peña, Penélope, Cohen, Roger, Fernández-Trincado, José G., Hayes, Christian R., Zasowski, Gail, Sobeck, Jennifer S., Majewski, Steven R., Chojnowski, S. D., De Lee, Nathan, Oelkers, Ryan J., Stringfellow, Guy S., Almeida, Andrés, Anguiano, Borja, Donor, John, Frinchaboy, Peter M., Hasselquist, Sten, Johnson, Jennifer A., Kollmeier, Juna A., Nidever, David L., Price-Whelan, Adrian. M., Rojas-Arriagada, Alvaro, Schultheis, Mathias, Shetrone, Matthew, Simon, Joshua D., Aerts, Conny, Borissova, Jura, Drout, Maria R., Geisler, Doug, Law, C. Y., Medina, Nicolás, Minniti, Dante, Monachesi, Antonela, Muñoz, Ricardo R., Poleski, Radosław, Roman-Lopes, Alexandre, Schlaufman, Kevin C., Stutz, Amelia M., Teske, Johanna, Tkachenko, Andrew, Van Saders, Jennifer L., Weinberger, Alycia, and Zoccali, Manuela
Abstract: APOGEE is a high-resolution (R sim 22,000), near-infrared, multi-epoch, spectroscopic survey of the Milky Way. The second generation of the APOGEE project, APOGEE-2, includes an expansion of the survey to the Southern Hemisphere called APOGEE-2S. This expansion enabled APOGEE to perform a fully panoramic mapping of all the main regions of the Milky Way; in particular, by operating in the H-band, APOGEE is uniquely able to probe the dust-hidden inner regions of the Milky Way that are best accessed from the Southern Hemisphere. In this paper we present the targeting strategy of APOGEE-2S, with special attention to documenting modifications to the original, previously published plan. The motivation for these changes is explained as well as an assessment of their effectiveness in achieving their intended scientific objective. In anticipation of this being the last paper detailing APOGEE targeting, we present an accounting of all such information complete through the end of the APOGEE-2S project; this includes several main survey programs dedicated to exploration of major stellar populations and regions of the Milky Way, as well as a full list of programs contributing to the APOGEE database through allocations of observing time by the Chilean National Time Allocation Committee (CNTAC) and the Carnegie Institution for Science (CIS). This work was presented along with a companion article, R. Beaton et al. (submitted; AAS29028), presenting the final target selection strategy adopted for APOGEE-2 in the Northern Hemisphere., Comment: 43 pages; 5 figures; 6 Tables; 1 Appendix; Submitted to Journal and Under Review; Posting to accompany papers using the SDSS-IV/APOGEE-2 Data Release 17 scheduled for December 2021
Published: 2021
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30. Multiwavelength properties of Miras

Author: Iwanek, Patryk, Kozłowski, Szymon, Gromadzki, Mariusz, Soszyński, Igor, Wrona, Marcin, Skowron, Jan, Ratajczak, Milena, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Poleski, Radosław, Mróz, Przemysław, Skowron, Dorota M., Rybicki, Krzysztof, Iwanek, Patryk, Kozłowski, Szymon, Gromadzki, Mariusz, Soszyński, Igor, Wrona, Marcin, Skowron, Jan, Ratajczak, Milena, Udalski, Andrzej, Szymański, Michał K., Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Poleski, Radosław, Mróz, Przemysław, Skowron, Dorota M., and Rybicki, Krzysztof
Abstract: We comprehensively study the variability of Miras in the Large Magellanic Cloud (LMC) by simultaneous analysing light curves in 14 bands in the range of 0.5$-$24 microns. We model over 20-years-long, high cadence $I$-band light curves collected by The Optical Gravitational Lensing Experiment (OGLE) and fit them to light curves collected in the remaining optical/near-infrared/mid-infrared bands to derive both the variability amplitude ratio and phase-lag as a function of wavelength. We show that the variability amplitude ratio declines with the increasing wavelength for both oxygen-rich (O-rich) and carbon-rich (C-rich) Miras, while the variability phase-lag increases slightly with the increasing wavelength. In a significant number of Miras, mostly the C-rich ones, the spectral energy distributions (SEDs) require a presence of a cool component (dust) in order to match the mid-IR data. Based on SED fits for a golden sample of 140 Miras, we calculated synthetic period-luminosity relations (PLRs) in 42 bands for the existing and future sky surveys that include OGLE, The VISTA Near-Infrared $YJK_\mathrm{s}$ Survey of the Magellanic Clouds System (VMC), Legacy Survey of Space and Time (LSST), Gaia, Spitzer, The Wide-field Infrared Survey Explorer (WISE), The James Webb Space Telescope (JWST), The Nancy Grace Roman Space Telescope (formerly WFIRST), and The Hubble Space Telescope (HST). We show that the synthetic PLR slope decreases with increasing wavelength for both the O-rich and C-rich Miras in the range of 0.1$-$40 microns. Finally, we show the location and motions of Miras on the color-magnitude (CMD) and color-color (CCD) diagrams., Comment: Accepted for publication in The Astrophysical Journal Supplement Series. 27 pages, 16 figures, 7 tables. The full machine readable tables will be available in the online journal just after publication
Published: 2021
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31. Determination of rotation periods for a large sample of asteroids from K2 Campaign 9

Author: Podlewska-Gaca, Edyta, Poleski, Radosław, Bartczak, Przemysław, McDonald, Iain, Pál, András, Podlewska-Gaca, Edyta, Poleski, Radosław, Bartczak, Przemysław, McDonald, Iain, and Pál, András
Abstract: Kepler mission is a powerful tool in the study the different types of astrophysical objects or events in the distant Universe. However, the spacecraft gives also the opportunity to study Solar System objects passing in the telescope field of view. The aim of this paper is to determine for the first time the rotation periods of a number of asteroids observed by the Kepler satellite during the K2 Campaign 9. Using publicly available data from Kepler mission we have used the Modified Causal Pixel Model (MCPM) code to perform the aperture-like and PRF-like photometry of 1026 asteroids. The results allowed us to determine the rotation periods for 188 asteroids. For asteroids with rotation periods previously measured, we compared the results and found very good agreement. There are additional 20 asteroids for which we obtained lower limits on rotation periods and in all cases these limits are at least 100 h., Comment: 24 pages, 8 figures, submitted to ApJS
Published: 2021
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32. Three microlensing planets with no caustic-crossing features

Author: Han, Cheongho, Udalski, Andrzej, Kim, Doeon, Lee, Chung-Uk, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Udalski, Andrzej, Kim, Doeon, Lee, Chung-Uk, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We search for microlensing planets with signals exhibiting no caustic-crossing features, considering the possibility that such signals may be missed due to their weak and featureless nature. For this purpose, we reexamine the lensing events found by the KMTNet survey before the 2019 season. From this investigation, we find two new planetary lensing events, KMT-2018-BLG-1976 and KMT-2018-BLG-1996. We also present the analysis of the planetary event OGLE-2019-BLG-0954, for which the planetary signal was known, but no detailed analysis has been presented before. We identify the genuineness of the planetary signals by checking various interpretations that can generate short-term anomalies in lensing light curves. From Bayesian analyses conducted with the constraint from available observables, we find that the host and planet masses are $(M_1, M_2)\sim (0.65~M_\odot, 2~M_{\rm J})$ for KMT-2018-BLG-1976L, $\sim (0.69~M_\odot, 1~M_{\rm J})$ for KMT-2018-BLG-1996L, and $\sim (0.80~M_\odot, 14~M_{\rm J})$ for OGLE-2019-BLG-0954L. The estimated distance to OGLE-2019-BLG-0954L, $3.63^{+1.22}_{-1.64}$~kpc, indicates that it is located in the disk, and the brightness expected from the mass and distance matches well the brightness of the blend, indicating that the lens accounts for most of the blended flux. The lens of OGLE-2019-BLG-0954 could be resolved from the source by conducting high-resolution follow-up observations in and after 2024., Comment: 11 pages, 14 figures
Published: 2021
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33. KMT-2018-BLG-1025Lb: microlensing super-Earth planet orbiting a low-mass star

Author: Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Doeon, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Han, Cheongho, Udalski, Andrzej, Lee, Chung-Uk, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn Kil, Kim, Doeon, Kim, Hyoun-Woo, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Kim, Chun-Hwey, Kim, Woong-Tae, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, and Wrona, Marcin
Abstract: We aim to find missing microlensing planets hidden in the unanalyzed lensing events of previous survey data. For this purpose, we conduct a systematic inspection of high-magnification microlensing events, with peak magnifications $A_{\rm peak}\gtrsim 30$, in the data collected from high-cadence surveys in and before the 2018 season. From this investigation, we identify an anomaly in the lensing light curve of the event KMT-2018-BLG-1025. The analysis of the light curve indicates that the anomaly is caused by a very low mass-ratio companion to the lens. We identify three degenerate solutions, in which the ambiguity between a pair of solutions (solutions B) is caused by the previously known close--wide degeneracy, and the degeneracy between these and the other solution (solution A) is a new type that has not been reported before. The estimated mass ratio between the planet and host is $q\sim 0.8\times 10^{-4}$ for the solution A and $q\sim 1.6\times 10^{-4}$ for the solutions B. From the Bayesian analysis conducted with measured observables, we estimate that the masses of the planet and host and the distance to the lens are $(M_{\rm p}, M_{\rm h}, D_{\rm L})\sim (6.1~M_\oplus, 0.22~M_\odot, 6.7~{\rm kpc})$ for the solution A and $\sim (4.4~M_\oplus, 0.08~M_\odot, 7.5~{\rm kpc})$ for the solutions B. The planet mass is in the category of a super-Earth regardless of the solutions, making the planet the eleventh super-Earth planet, with masses lying between those of Earth and the Solar system's ice giants, discovered by microlensing., Comment: 10 pages, 10 figures, 5 tables
Published: 2021
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34. KMT-2019-BLG-1339L: an M Dwarf with a Giant Planet or a Companion Near the Planet/Brown Dwarf Boundary

Author: Han, Cheongho, Kim, Doeon, Udalski, Andrzej, Gould, Andrew, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szyma'nski, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Kim, Doeon, Udalski, Andrzej, Gould, Andrew, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szyma'nski, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We analyze KMT-2019-BLG-1339, a microlensing event with an obvious but incompletely resolved brief anomaly feature around the peak of the light curve. Although the origin of the anomaly is identified to be a companion to the lens with a low mass ratio $q$, the interpretation is subject to two different degeneracy types. The first type is the ambiguity in $\rho$, representing the angular source radius scaled to the angular radius of the Einstein ring, $\theta_{\rm E}$, and the other is the $s\leftrightarrow s^{-1}$ degeneracy. The former type, `finite-source degeneracy', causes ambiguities in both $s$ and $q$, while the latter induces an ambiguity only in $s$. Here $s$ denotes the separation (in units of $\theta_{\rm E}$) in projection between the lens components. We estimate that the lens components have masses $(M_1, M_2)\sim (0.27^{+0.36}_{-0.15}~M_\odot, 11^{+16}_{-7}~M_{\rm J})$ and $\sim (0.48^{+0.40}_{-0.28}~M_\odot, 1.3^{+1.1}_{-0.7}~M_{\rm J})$ according to the two solutions subject to the finite-source degeneracy, indicating that the lens comprises an M dwarf and a companion with a mass around the planet/brown dwarf boundary or a Jovian-mass planet. It is possible to lift the finite-source degeneracy by conducting future observations utilizing a high resolution instrument because the relative lens-source proper motion predicted by the solutions are widely different., Comment: 8 pages, 6 figures
Published: 2020
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35. KMT-2019-BLG-1339L: an M Dwarf with a Giant Planet or a Companion Near the Planet/Brown Dwarf Boundary

Author: Han, Cheongho, Kim, Doeon, Udalski, Andrzej, Gould, Andrew, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szyma'nski, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Han, Cheongho, Kim, Doeon, Udalski, Andrzej, Gould, Andrew, Albrow, Michael D., Chung, Sun-Ju, Hwang, Kyu-Ha, Jung, Youn Kil, Lee, Chung-Uk, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Szyma'nski, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, and Gromadzki, Mariusz
Abstract: We analyze KMT-2019-BLG-1339, a microlensing event with an obvious but incompletely resolved brief anomaly feature around the peak of the light curve. Although the origin of the anomaly is identified to be a companion to the lens with a low mass ratio $q$, the interpretation is subject to two different degeneracy types. The first type is the ambiguity in $\rho$, representing the angular source radius scaled to the angular radius of the Einstein ring, $\theta_{\rm E}$, and the other is the $s\leftrightarrow s^{-1}$ degeneracy. The former type, `finite-source degeneracy', causes ambiguities in both $s$ and $q$, while the latter induces an ambiguity only in $s$. Here $s$ denotes the separation (in units of $\theta_{\rm E}$) in projection between the lens components. We estimate that the lens components have masses $(M_1, M_2)\sim (0.27^{+0.36}_{-0.15}~M_\odot, 11^{+16}_{-7}~M_{\rm J})$ and $\sim (0.48^{+0.40}_{-0.28}~M_\odot, 1.3^{+1.1}_{-0.7}~M_{\rm J})$ according to the two solutions subject to the finite-source degeneracy, indicating that the lens comprises an M dwarf and a companion with a mass around the planet/brown dwarf boundary or a Jovian-mass planet. It is possible to lift the finite-source degeneracy by conducting future observations utilizing a high resolution instrument because the relative lens-source proper motion predicted by the solutions are widely different., Comment: 8 pages, 6 figures
Published: 2020
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36. Supersoft X-ray emission from a white dwarf binary not powered by nuclear fusion

Author: Maccarone, Thomas J., Nelson, Thomas J., Brown, Peter J., Mukai, Koji, Charles, Philip A., Rajoelimanana, Andry, Buckley, David A. H., Strader, Jay, Chomiuk, Laura, Britt, Christopher T., Jha, Saurabh W., Mróz, Przemek, Udalski, Andrzej, Szymański, Michal K., Soszyński, Igor, Poleski, Radosław, Kozłowski, Szymon, Pietrukowicz, Paweł, Skowron, Jan, Ulaczyk, Krzysztof, Maccarone, Thomas J., Nelson, Thomas J., Brown, Peter J., Mukai, Koji, Charles, Philip A., Rajoelimanana, Andry, Buckley, David A. H., Strader, Jay, Chomiuk, Laura, Britt, Christopher T., Jha, Saurabh W., Mróz, Przemek, Udalski, Andrzej, Szymański, Michal K., Soszyński, Igor, Poleski, Radosław, Kozłowski, Szymon, Pietrukowicz, Paweł, Skowron, Jan, and Ulaczyk, Krzysztof
Abstract: Supersoft X-ray sources are stellar objects which emit X-rays with temperatures of about 1 million Kelvin and luminosities well in excess of what can be produced by stellar coronae. It has generally been presumed that the objects in this class are binary star systems in which mass transfer leads to nuclear fusion on the surface of a white dwarf. Classical novae, the runaway fusion events on the surfaces of white dwarfs, generally have supersoft phases, and it is often stated that the bright steady supersoft X-ray sources seen from white dwarfs accreting mass at a high rate are undergoing steady nuclear fusion. In this letter, we report the discovery of a transient supersoft source in the Small Magellanic Cloud without any signature of nuclear fusion having taken place. This discovery indicates that the X-ray emission probably comes from a "spreading layer" - a belt on the surface of the white dwarf near the inner edge of the accretion disk in which a large fraction of the total accretion energy is emitted - and (albeit more tentatively) that the accreting white dwarf is relatively massive. We thus establish that the presence of a supersoft source cannot always be used as a tracer of nuclear fusion, in contradiction with decades-old consensus about the nature of supersoft emission., Comment: 15 pages, 4 figures, published in Nature Astronomy
Published: 2019

37. OGLE-2015-BLG-1649Lb: A gas giant planet around a low-mass dwarf

Author: Nagakane, Masayuki, Lee, Chien-Hsiu, Koshimoto, Naoki, Suzuki, Daisuke, Udalski, Andrzej, Beaulieu, Jean-Philippe, Sumi, Takahiro, Bennett, David, Bond, Ian A., Rattenbury, Nicholas J., Bachelet, Etienne, Dominik, Martin, Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Donachie, Martin, Fujii, H., Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kamei, Y., Kondo, Iona, Li, Man Cheung Alex, Matsubara, Y., Matsuo, Taro, Miyazaki, Shota, Muraki, Yasushi, Ranc, Clément, Shibai, Hiroshi, Suematsu, Haruno, Sullivan, Denis, Tristram, P., Yamakawa, T., Yonehara, A., Mróz, P., Poleski, Radosław, Skowron, Jan, Szymański, M., Soszyński, I., Pietrukowicz, Pawel, Kozłowski, Szymon, Ulaczyk, Krzysztof, Bramich, Dan, Cassan, Arnaud, Jaimes, R., Horne, K., Hundertmark, Markus, Mao, Shude, Menzies, John, Schmidt, R., Snodgrass, Colin, Steele, Iain, Street, Rachel, Tsapras, Yiannis, Wambsganss, Joachim, Jørgensen, Uffe, Bozza, Valerio, Longã, P., Peixinho, Nuno, Skottfelt, Jesper, Southworth, John, Andersen, M. I., Burgdorf, M., D'Ago, Giuseppe, Evans, Daniel, Hinse, Tobias, Korhonen, Heidi, Rabus, Markus, Rahvar, Sohrab, Nagakane, Masayuki, Lee, Chien-Hsiu, Koshimoto, Naoki, Suzuki, Daisuke, Udalski, Andrzej, Beaulieu, Jean-Philippe, Sumi, Takahiro, Bennett, David, Bond, Ian A., Rattenbury, Nicholas J., Bachelet, Etienne, Dominik, Martin, Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Donachie, Martin, Fujii, H., Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kamei, Y., Kondo, Iona, Li, Man Cheung Alex, Matsubara, Y., Matsuo, Taro, Miyazaki, Shota, Muraki, Yasushi, Ranc, Clément, Shibai, Hiroshi, Suematsu, Haruno, Sullivan, Denis, Tristram, P., Yamakawa, T., Yonehara, A., Mróz, P., Poleski, Radosław, Skowron, Jan, Szymański, M., Soszyński, I., Pietrukowicz, Pawel, Kozłowski, Szymon, Ulaczyk, Krzysztof, Bramich, Dan, Cassan, Arnaud, Jaimes, R., Horne, K., Hundertmark, Markus, Mao, Shude, Menzies, John, Schmidt, R., Snodgrass, Colin, Steele, Iain, Street, Rachel, Tsapras, Yiannis, Wambsganss, Joachim, Jørgensen, Uffe, Bozza, Valerio, Longã, P., Peixinho, Nuno, Skottfelt, Jesper, Southworth, John, Andersen, M. I., Burgdorf, M., D'Ago, Giuseppe, Evans, Daniel, Hinse, Tobias, Korhonen, Heidi, Rabus, Markus, and Rahvar, Sohrab
Abstract: We report the discovery of an exoplanet in microlensing event OGLE-2015-BLG-1649. The planet/host-star mass ratio is $q =7.2 \times 10^{-3}$ and the projected separation normalized by the Einstein radius is $s = 0.9$. The upper limit of the lens flux is obtained from adaptive optics observations by IRCS/Subaru, which excludes the probability of a G-dwarf or more massive host star and helps to put a tighter constraint on the lens mass as well as commenting on the formation scenarios of giant planets orbiting low-mass stars. We conduct a Bayesian analysis including constraints on the lens flux to derive the probability distribution of the physical parameters of the lens system. We thereby find that the masses of the host star and planet are $M_{L} = 0.34 \pm 0.19 M_{\odot}$ and $M_{p} = 2.5^{+1.5}_{-1.4} M_{Jup}$, respectively. The distance to the system is $D_{L} = 4.23^{+1.51}_{-1.64}$kpc. The projected star-planet separation is $a_{\perp} = 2.07^{+0.65}_{-0.77}$AU. The lens-source relative proper motion of the event is quite high, at $\sim 7.1 \, {\rm mas/yr}$. Therefore, we may be able to determine the lens physical parameters uniquely or place much stronger constraints on them by measuring the color-dependent centroid shift and/or the image elongation with additional high resolution imaging already a few years from now., Comment: 24 pages, 5 figures, 3 tables. Accepted for publication in AJ
Published: 2019
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38. OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

Author: Li, Shun-Sheng, Zang, Weicheng, Udalski, Andrzej, Shvartzvald, Yossi, Huber, Daniel, Lee, Chung-Uk, Sumi, Takahiro, Gould, Andrew, Mao, Shude, Fouqué, Pascal, Wang, Tianshu, Dong, Subo, Jørgensen, Uffe G., Cole, Andrew, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Yee, Jennifer C., Novati, Sebastiano Calchi, Beichman, Charles A., Bryden, Geoffery, Carey, Sean, Gaudi, B. Scott, Henderson, Calen B., Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Han, Cheongho, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Bond, Ian A., Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Christie, Grant, Drummond, John, Green, Jonathan, Hennerley, Steve, Natusch, Tim, Porritt, Ian, Bachelet, Etienne, Maoz, Dan, Street, Rachel A., Tsapras, Yiannis, Bozza, Valerio, Dominik, Martin, Hundertmark, Markus, Peixinho, Nuno, Sajadian, Sedighe, Burgdorf, Martin J., Evans, Daniel F., Jaimes, Roberto Figuera, Fujii, Yuri I., Haikala, Lauri K., Helling, Christiane, Henning, Thomas, Hinse, Tobias C., Mancini, Luigi, Longa-Peña, Penelope, Rahvar, Sohrab, Rabus, Markus, Skottfelt, Jesper, Snodgrass, Colin, Southworth, John, Unda-Sanzana, Eduardo, von Essen, Carolina, Beaulieu, Jean-Phillipe, Blackman, Joshua, Hill, Kym, Li, Shun-Sheng, Zang, Weicheng, Udalski, Andrzej, Shvartzvald, Yossi, Huber, Daniel, Lee, Chung-Uk, Sumi, Takahiro, Gould, Andrew, Mao, Shude, Fouqué, Pascal, Wang, Tianshu, Dong, Subo, Jørgensen, Uffe G., Cole, Andrew, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Yee, Jennifer C., Novati, Sebastiano Calchi, Beichman, Charles A., Bryden, Geoffery, Carey, Sean, Gaudi, B. Scott, Henderson, Calen B., Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Han, Cheongho, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Bond, Ian A., Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Christie, Grant, Drummond, John, Green, Jonathan, Hennerley, Steve, Natusch, Tim, Porritt, Ian, Bachelet, Etienne, Maoz, Dan, Street, Rachel A., Tsapras, Yiannis, Bozza, Valerio, Dominik, Martin, Hundertmark, Markus, Peixinho, Nuno, Sajadian, Sedighe, Burgdorf, Martin J., Evans, Daniel F., Jaimes, Roberto Figuera, Fujii, Yuri I., Haikala, Lauri K., Helling, Christiane, Henning, Thomas, Hinse, Tobias C., Mancini, Luigi, Longa-Peña, Penelope, Rahvar, Sohrab, Rabus, Markus, Skottfelt, Jesper, Snodgrass, Colin, Southworth, John, Unda-Sanzana, Eduardo, von Essen, Carolina, Beaulieu, Jean-Phillipe, Blackman, Joshua, and Hill, Kym
Abstract: We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average timescale of $\sim 9$ d. The asteroseismic analysis also provides us source properties including the source angular size ($\sim 27~\mu{\rm as}$) and distance ($\sim 11.5$ kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian Processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional $\chi^2$ minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a $\sim 0.045~M_{\odot}$ brown dwarf at distance $\sim 9.0$ kpc, or a $\sim 0.073~M_{\odot}$ ultracool dwarf at distance $\sim 9.8$ kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a $\sim 35$ per cent probability for the lens to be a bulge object and $\sim 65$ per cent to be a background disc object., Comment: 18 pages, 4 figures, 5 tables. Revised to match version published in MNRAS
Published: 2019
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39. Supersoft X-ray emission from a white dwarf binary not powered by nuclear fusion

Author: Maccarone, Thomas J., Nelson, Thomas J., Brown, Peter J., Mukai, Koji, Charles, Philip A., Rajoelimanana, Andry, Buckley, David A. H., Strader, Jay, Chomiuk, Laura, Britt, Christopher T., Jha, Saurabh W., Mróz, Przemek, Udalski, Andrzej, Szymański, Michal K., Soszyński, Igor, Poleski, Radosław, Kozłowski, Szymon, Pietrukowicz, Paweł, Skowron, Jan, Ulaczyk, Krzysztof, Maccarone, Thomas J., Nelson, Thomas J., Brown, Peter J., Mukai, Koji, Charles, Philip A., Rajoelimanana, Andry, Buckley, David A. H., Strader, Jay, Chomiuk, Laura, Britt, Christopher T., Jha, Saurabh W., Mróz, Przemek, Udalski, Andrzej, Szymański, Michal K., Soszyński, Igor, Poleski, Radosław, Kozłowski, Szymon, Pietrukowicz, Paweł, Skowron, Jan, and Ulaczyk, Krzysztof
Abstract: Supersoft X-ray sources are stellar objects which emit X-rays with temperatures of about 1 million Kelvin and luminosities well in excess of what can be produced by stellar coronae. It has generally been presumed that the objects in this class are binary star systems in which mass transfer leads to nuclear fusion on the surface of a white dwarf. Classical novae, the runaway fusion events on the surfaces of white dwarfs, generally have supersoft phases, and it is often stated that the bright steady supersoft X-ray sources seen from white dwarfs accreting mass at a high rate are undergoing steady nuclear fusion. In this letter, we report the discovery of a transient supersoft source in the Small Magellanic Cloud without any signature of nuclear fusion having taken place. This discovery indicates that the X-ray emission probably comes from a "spreading layer" - a belt on the surface of the white dwarf near the inner edge of the accretion disk in which a large fraction of the total accretion energy is emitted - and (albeit more tentatively) that the accreting white dwarf is relatively massive. We thus establish that the presence of a supersoft source cannot always be used as a tracer of nuclear fusion, in contradiction with decades-old consensus about the nature of supersoft emission., Comment: 15 pages, 4 figures, published in Nature Astronomy
Published: 2019

40. OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

Author: Li, Shun-Sheng, Zang, Weicheng, Udalski, Andrzej, Shvartzvald, Yossi, Huber, Daniel, Lee, Chung-Uk, Sumi, Takahiro, Gould, Andrew, Mao, Shude, Fouqué, Pascal, Wang, Tianshu, Dong, Subo, Jørgensen, Uffe G., Cole, Andrew, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Yee, Jennifer C., Novati, Sebastiano Calchi, Beichman, Charles A., Bryden, Geoffery, Carey, Sean, Gaudi, B. Scott, Henderson, Calen B., Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Han, Cheongho, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Bond, Ian A., Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Christie, Grant, Drummond, John, Green, Jonathan, Hennerley, Steve, Natusch, Tim, Porritt, Ian, Bachelet, Etienne, Maoz, Dan, Street, Rachel A., Tsapras, Yiannis, Bozza, Valerio, Dominik, Martin, Hundertmark, Markus, Peixinho, Nuno, Sajadian, Sedighe, Burgdorf, Martin J., Evans, Daniel F., Jaimes, Roberto Figuera, Fujii, Yuri I., Haikala, Lauri K., Helling, Christiane, Henning, Thomas, Hinse, Tobias C., Mancini, Luigi, Longa-Peña, Penelope, Rahvar, Sohrab, Rabus, Markus, Skottfelt, Jesper, Snodgrass, Colin, Southworth, John, Unda-Sanzana, Eduardo, von Essen, Carolina, Beaulieu, Jean-Phillipe, Blackman, Joshua, Hill, Kym, Li, Shun-Sheng, Zang, Weicheng, Udalski, Andrzej, Shvartzvald, Yossi, Huber, Daniel, Lee, Chung-Uk, Sumi, Takahiro, Gould, Andrew, Mao, Shude, Fouqué, Pascal, Wang, Tianshu, Dong, Subo, Jørgensen, Uffe G., Cole, Andrew, Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radosław, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Yee, Jennifer C., Novati, Sebastiano Calchi, Beichman, Charles A., Bryden, Geoffery, Carey, Sean, Gaudi, B. Scott, Henderson, Calen B., Zhu, Wei, Albrow, Michael D., Chung, Sun-Ju, Han, Cheongho, Hwang, Kyu-Ha, Jung, Youn Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Bond, Ian A., Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Christie, Grant, Drummond, John, Green, Jonathan, Hennerley, Steve, Natusch, Tim, Porritt, Ian, Bachelet, Etienne, Maoz, Dan, Street, Rachel A., Tsapras, Yiannis, Bozza, Valerio, Dominik, Martin, Hundertmark, Markus, Peixinho, Nuno, Sajadian, Sedighe, Burgdorf, Martin J., Evans, Daniel F., Jaimes, Roberto Figuera, Fujii, Yuri I., Haikala, Lauri K., Helling, Christiane, Henning, Thomas, Hinse, Tobias C., Mancini, Luigi, Longa-Peña, Penelope, Rahvar, Sohrab, Rabus, Markus, Skottfelt, Jesper, Snodgrass, Colin, Southworth, John, Unda-Sanzana, Eduardo, von Essen, Carolina, Beaulieu, Jean-Phillipe, Blackman, Joshua, and Hill, Kym
Abstract: We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average timescale of $\sim 9$ d. The asteroseismic analysis also provides us source properties including the source angular size ($\sim 27~\mu{\rm as}$) and distance ($\sim 11.5$ kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian Processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional $\chi^2$ minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a $\sim 0.045~M_{\odot}$ brown dwarf at distance $\sim 9.0$ kpc, or a $\sim 0.073~M_{\odot}$ ultracool dwarf at distance $\sim 9.8$ kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a $\sim 35$ per cent probability for the lens to be a bulge object and $\sim 65$ per cent to be a background disc object., Comment: 18 pages, 4 figures, 5 tables. Revised to match version published in MNRAS
Published: 2019
Full Text: View/download PDF

41. OGLE-2015-BLG-1649Lb: A gas giant planet around a low-mass dwarf

Author: Nagakane, Masayuki, Lee, Chien-Hsiu, Koshimoto, Naoki, Suzuki, Daisuke, Udalski, Andrzej, Beaulieu, Jean-Philippe, Sumi, Takahiro, Bennett, David, Bond, Ian A., Rattenbury, Nicholas J., Bachelet, Etienne, Dominik, Martin, Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Donachie, Martin, Fujii, H., Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kamei, Y., Kondo, Iona, Li, Man Cheung Alex, Matsubara, Y., Matsuo, Taro, Miyazaki, Shota, Muraki, Yasushi, Ranc, Clément, Shibai, Hiroshi, Suematsu, Haruno, Sullivan, Denis, Tristram, P., Yamakawa, T., Yonehara, A., Mróz, P., Poleski, Radosław, Skowron, Jan, Szymański, M., Soszyński, I., Pietrukowicz, Pawel, Kozłowski, Szymon, Ulaczyk, Krzysztof, Bramich, Dan, Cassan, Arnaud, Jaimes, R., Horne, K., Hundertmark, Markus, Mao, Shude, Menzies, John, Schmidt, R., Snodgrass, Colin, Steele, Iain, Street, Rachel, Tsapras, Yiannis, Wambsganss, Joachim, Jørgensen, Uffe, Bozza, Valerio, Longã, P., Peixinho, Nuno, Skottfelt, Jesper, Southworth, John, Andersen, M. I., Burgdorf, M., D'Ago, Giuseppe, Evans, Daniel, Hinse, Tobias, Korhonen, Heidi, Rabus, Markus, Rahvar, Sohrab, Nagakane, Masayuki, Lee, Chien-Hsiu, Koshimoto, Naoki, Suzuki, Daisuke, Udalski, Andrzej, Beaulieu, Jean-Philippe, Sumi, Takahiro, Bennett, David, Bond, Ian A., Rattenbury, Nicholas J., Bachelet, Etienne, Dominik, Martin, Abe, Fumio, Barry, Richard, Bhattacharya, Aparna, Donachie, Martin, Fujii, H., Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kamei, Y., Kondo, Iona, Li, Man Cheung Alex, Matsubara, Y., Matsuo, Taro, Miyazaki, Shota, Muraki, Yasushi, Ranc, Clément, Shibai, Hiroshi, Suematsu, Haruno, Sullivan, Denis, Tristram, P., Yamakawa, T., Yonehara, A., Mróz, P., Poleski, Radosław, Skowron, Jan, Szymański, M., Soszyński, I., Pietrukowicz, Pawel, Kozłowski, Szymon, Ulaczyk, Krzysztof, Bramich, Dan, Cassan, Arnaud, Jaimes, R., Horne, K., Hundertmark, Markus, Mao, Shude, Menzies, John, Schmidt, R., Snodgrass, Colin, Steele, Iain, Street, Rachel, Tsapras, Yiannis, Wambsganss, Joachim, Jørgensen, Uffe, Bozza, Valerio, Longã, P., Peixinho, Nuno, Skottfelt, Jesper, Southworth, John, Andersen, M. I., Burgdorf, M., D'Ago, Giuseppe, Evans, Daniel, Hinse, Tobias, Korhonen, Heidi, Rabus, Markus, and Rahvar, Sohrab
Abstract: We report the discovery of an exoplanet in microlensing event OGLE-2015-BLG-1649. The planet/host-star mass ratio is $q =7.2 \times 10^{-3}$ and the projected separation normalized by the Einstein radius is $s = 0.9$. The upper limit of the lens flux is obtained from adaptive optics observations by IRCS/Subaru, which excludes the probability of a G-dwarf or more massive host star and helps to put a tighter constraint on the lens mass as well as commenting on the formation scenarios of giant planets orbiting low-mass stars. We conduct a Bayesian analysis including constraints on the lens flux to derive the probability distribution of the physical parameters of the lens system. We thereby find that the masses of the host star and planet are $M_{L} = 0.34 \pm 0.19 M_{\odot}$ and $M_{p} = 2.5^{+1.5}_{-1.4} M_{Jup}$, respectively. The distance to the system is $D_{L} = 4.23^{+1.51}_{-1.64}$kpc. The projected star-planet separation is $a_{\perp} = 2.07^{+0.65}_{-0.77}$AU. The lens-source relative proper motion of the event is quite high, at $\sim 7.1 \, {\rm mas/yr}$. Therefore, we may be able to determine the lens physical parameters uniquely or place much stronger constraints on them by measuring the color-dependent centroid shift and/or the image elongation with additional high resolution imaging already a few years from now., Comment: 24 pages, 5 figures, 3 tables. Accepted for publication in AJ
Published: 2019
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42. OGLE-2015-BLG-1670Lb: A Cold Neptune beyond the Snow Line in the Provisional WFIRST Microlensing Survey Field

Author: Ranc, Clément, Bennett, David P., Hirao, Yuki, Udalski, Andrzej, Han, Cheongho, Bond, Ian A., Yee, Jennifer C., Collaboration, The KMTNet, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn-Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Zang, Weicheng, Zhu, Wei, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yong-Seok, Park, Byeong-Gon, Pogge, Richard W., Collaboration, The MOA, Abe, Fumio, Barry, Richard K., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Nagakane, Masayuki, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Collaboration, The OGLE, Poleski, Radosław, Mróz, Przemek, Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Kozłowski, Szymon, Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Ranc, Clément, Bennett, David P., Hirao, Yuki, Udalski, Andrzej, Han, Cheongho, Bond, Ian A., Yee, Jennifer C., Collaboration, The KMTNet, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn-Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Zang, Weicheng, Zhu, Wei, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yong-Seok, Park, Byeong-Gon, Pogge, Richard W., Collaboration, The MOA, Abe, Fumio, Barry, Richard K., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Nagakane, Masayuki, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Collaboration, The OGLE, Poleski, Radosław, Mróz, Przemek, Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Kozłowski, Szymon, Pietrukowicz, Paweł, and Ulaczyk, Krzysztof
Abstract: We present the analysis of the microlensing event OGLE-2015-BLG-1670, detected in a high-extinction field, very close to the Galactic plane. Due to the dust extinction along the line of sight, this event was too faint to be detected before it reached the peak of magnification. The microlensing light-curve models indicate a high-magnification event with a maximum of $A_\mathrm{max}\gtrsim200$, very sensitive to planetary deviations. An anomaly in the light curve has been densely observed by the microlensing surveys MOA, KMTNet, and OGLE. From the light-curve modeling, we find a planetary anomaly characterized by a planet-to-host mass ratio, $q=\left(1.00^{+0.18}_{-0.16}\right)\times 10^{-4}$, at the peak recently identified in the mass-ratio function of microlensing planets. Thus, this event is interesting to include in future statistical studies about planet demography. We have explored the possible degeneracies and find two competing planetary models resulting from the $s\leftrightarrow1/s$ degeneracy. However, because the projected separation is very close to $s=1$, the physical implications for the planet for the two solutions are quite similar, except for the value of $s$. By combining the light-curve parameters with a Galactic model, we have estimated the planet mass $M_2=17.9^{+9.6}_{-8.8}\,\mathrm{M}_\oplus$ and the lens distance $D_\mathrm{L}=6.7^{+1.0}_{-1.3}\,\mathrm{kpc}$, corresponding to a Neptune-mass planet close to the Galactic bulge. Such events with a low absolute latitude ($|b|\approx 1.1\,\mathrm{deg}$) are subject to both high extinction and more uncertain source distances, two factors that may affect the mass measurements in the provisional Wide Field Infrared Survey Telescope fields. More events are needed to investigate the potential trade-off between the higher lensing rate and the difficulty in measuring masses in these low-latitude fields., Comment: 30 pages, 8 figures, 5 tables. Typos corrected and section 3.2.3 added. Version accepted for publication in The Astronomical Journal
Published: 2018
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43. OGLE-2014-BLG-0962 and the First Statistical Validation of Bayesian Priors for Galactic Microlensing

Author: Shan, Yutong, Yee, Jennifer C., Udalski, Andrzej, Bond, Ian A., Shvartzvald, Yossi, Shin, In-Gu, Jung, Youn-Kil, Novati, Sebastiano Calchi, Beichman, Charles A., Carey, Sean, Gaudi, B. Scott, Gould, Andrew, Pogge, Richard W., Poleski, Radosław, Skowron, Jan, Kozłowski, Szymon, Mróz, Przemysław, Pietrukowicz, Paweł, Szymański, Michał K., Soszyński, Igor, Ulaczyk, Krzysztof, Wyrzykowski, Łukasz, Abe, Fumio, Barry, Richard K., Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Maoz, Dan, Kaspi, Shai, Friedmann, Matan, Shan, Yutong, Yee, Jennifer C., Udalski, Andrzej, Bond, Ian A., Shvartzvald, Yossi, Shin, In-Gu, Jung, Youn-Kil, Novati, Sebastiano Calchi, Beichman, Charles A., Carey, Sean, Gaudi, B. Scott, Gould, Andrew, Pogge, Richard W., Poleski, Radosław, Skowron, Jan, Kozłowski, Szymon, Mróz, Przemysław, Pietrukowicz, Paweł, Szymański, Michał K., Soszyński, Igor, Ulaczyk, Krzysztof, Wyrzykowski, Łukasz, Abe, Fumio, Barry, Richard K., Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Maoz, Dan, Kaspi, Shai, and Friedmann, Matan
Abstract: OGLE-2014-BLG-0962 (OB140962) is a stellar binary microlensing event that was well-covered by observations from the Spitzer satellite as well as ground-based surveys. Modelling yields a unique physical solution: a mid-M+M-dwarf binary with $M_{\rm prim} = 0.20 \pm 0.01 M_\odot$ and $M_{\rm sec} = 0.16 \pm 0.01 M_\odot$, with projected separation of $2.0 \pm 0.3$ AU. The lens is only $D_{\rm LS} = 0.41 \pm 0.06$ kpc in front of the source, making OB140962 a bulge lens and the most distant Spitzer binary lens to date. In contrast, because the Einstein radius ($\theta_{\rm E} = 0.143 \pm 0.007$ mas) is unusually small, a standard Bayesian analysis, conducted in the absence of parallax information, would predict a brown dwarf binary. We test the accuracy of Bayesian analysis over a set of Spitzer lenses, finding overall good agreement throughout the sample. We also illustrate the methodology for probing the Galactic distribution of planets by comparing the cumulative distance distribution of the Spitzer 2-body lenses to that of the Spitzer single lenses., Comment: 15 pages, 7 figures, 5 tables; submitted to ApJ
Published: 2018

44. Continuum Reverberation Mapping of the Accretion Disks in Two Seyfert 1 Galaxies

Author: Fausnaugh, M. M., Starkey, D. A., Horne, Keith, Kochanek, C. S., Peterson, B. M., Bentz, M. C., Denney, K. D., Grier, C. J., Grupe, D., Pogge, R. W., DeRosa, G., Adams, S. M., Barth, A. J., Beatty, Thomas G., Bhattacharjee, A., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brown, Jacob E., Brown, Jonathan S., Brotherton, M. S., Coker, C. T., Crawford, S. M., Croxall, K. V., Eftekharzadeh, Sarah, Eracleous, Michael, Joner, M. D., Henderson, C. B., Holoien, T. W. -S., Hutchison, T., Kaspi, Shai, Kim, S., King, Anthea L., Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F., Manne-Nicholas, E. R., Mason, M., Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R., Nazarov, S. V., Nguyen, M. L., Okhmat, D. N., Onken, ChristopherA., Ou-Yang, B., Pancoast, A., Pei, L., Penny, Matthew T., Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E., Runnoe, Jessie, Sand, David J., Schimoia, Jaderson S., Sergeev, S. G., Shappee, B. J., Simonian, Gregory V., Somers, Garrett, Spencer, M., Stevens, Daniel J., Tayar, Jamie, Treu, T., Valenti, Stefano, VanSaders, J., VillanuevaJr., S., Villforth, C., Weiss, Yaniv, Winkler, H., Zhu, W., Fausnaugh, M. M., Starkey, D. A., Horne, Keith, Kochanek, C. S., Peterson, B. M., Bentz, M. C., Denney, K. D., Grier, C. J., Grupe, D., Pogge, R. W., DeRosa, G., Adams, S. M., Barth, A. J., Beatty, Thomas G., Bhattacharjee, A., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brown, Jacob E., Brown, Jonathan S., Brotherton, M. S., Coker, C. T., Crawford, S. M., Croxall, K. V., Eftekharzadeh, Sarah, Eracleous, Michael, Joner, M. D., Henderson, C. B., Holoien, T. W. -S., Hutchison, T., Kaspi, Shai, Kim, S., King, Anthea L., Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F., Manne-Nicholas, E. R., Mason, M., Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R., Nazarov, S. V., Nguyen, M. L., Okhmat, D. N., Onken, ChristopherA., Ou-Yang, B., Pancoast, A., Pei, L., Penny, Matthew T., Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E., Runnoe, Jessie, Sand, David J., Schimoia, Jaderson S., Sergeev, S. G., Shappee, B. J., Simonian, Gregory V., Somers, Garrett, Spencer, M., Stevens, Daniel J., Tayar, Jamie, Treu, T., Valenti, Stefano, VanSaders, J., VillanuevaJr., S., Villforth, C., Weiss, Yaniv, Winkler, H., and Zhu, W.
Abstract: We present optical continuum lags for two Seyfert 1 galaxies, MCG+08-11-011 and NGC 2617, using monitoring data from a reverberation mapping campaign carried out in 2014. Our light curves span the ugriz filters over four months, with median cadences of 1.0 and 0.6 days for MCG+08-11-011 and NGC\,2617, respectively, combined with roughly daily X-ray and near-UV data from Swift for NGC 2617. We find lags consistent with geometrically thin accretion-disk models that predict a lag-wavelength relation of $\tau \propto \lambda^{4/3}$. However, the observed lags are larger than predictions based on standard thin-disk theory by factors of 3.3 for MCG+08-11-011 and 2.3 for NGC\,2617. These differences can be explained if the mass accretion rates are larger than inferred from the optical luminosity by a factor of 4.3 in MCG+08-11-011 and a factor of 1.3 in NGC\,2617, although uncertainty in the SMBH masses determines the significance of this result. While the X-ray variability in NGC\,2617 precedes the UV/optical variability, the long 2.6 day lag is problematic for coronal reprocessing models., Comment: Accepted to ApJ, please send comments to faus@mit.edu. 24 pages, 8 figures
Published: 2018
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45. OGLE-2015-BLG-1670Lb: A Cold Neptune beyond the Snow Line in the Provisional WFIRST Microlensing Survey Field

Author: Ranc, Clément, Bennett, David P., Hirao, Yuki, Udalski, Andrzej, Han, Cheongho, Bond, Ian A., Yee, Jennifer C., Collaboration, The KMTNet, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn-Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Zang, Weicheng, Zhu, Wei, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yong-Seok, Park, Byeong-Gon, Pogge, Richard W., Collaboration, The MOA, Abe, Fumio, Barry, Richard K., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Nagakane, Masayuki, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Collaboration, The OGLE, Poleski, Radosław, Mróz, Przemek, Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Kozłowski, Szymon, Pietrukowicz, Paweł, Ulaczyk, Krzysztof, Ranc, Clément, Bennett, David P., Hirao, Yuki, Udalski, Andrzej, Han, Cheongho, Bond, Ian A., Yee, Jennifer C., Collaboration, The KMTNet, Albrow, Michael D., Chung, Sun-Ju, Gould, Andrew, Hwang, Kyu-Ha, Jung, Youn-Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Zang, Weicheng, Zhu, Wei, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yong-Seok, Park, Byeong-Gon, Pogge, Richard W., Collaboration, The MOA, Abe, Fumio, Barry, Richard K., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Nagakane, Masayuki, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Collaboration, The OGLE, Poleski, Radosław, Mróz, Przemek, Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Kozłowski, Szymon, Pietrukowicz, Paweł, and Ulaczyk, Krzysztof
Abstract: We present the analysis of the microlensing event OGLE-2015-BLG-1670, detected in a high-extinction field, very close to the Galactic plane. Due to the dust extinction along the line of sight, this event was too faint to be detected before it reached the peak of magnification. The microlensing light-curve models indicate a high-magnification event with a maximum of $A_\mathrm{max}\gtrsim200$, very sensitive to planetary deviations. An anomaly in the light curve has been densely observed by the microlensing surveys MOA, KMTNet, and OGLE. From the light-curve modeling, we find a planetary anomaly characterized by a planet-to-host mass ratio, $q=\left(1.00^{+0.18}_{-0.16}\right)\times 10^{-4}$, at the peak recently identified in the mass-ratio function of microlensing planets. Thus, this event is interesting to include in future statistical studies about planet demography. We have explored the possible degeneracies and find two competing planetary models resulting from the $s\leftrightarrow1/s$ degeneracy. However, because the projected separation is very close to $s=1$, the physical implications for the planet for the two solutions are quite similar, except for the value of $s$. By combining the light-curve parameters with a Galactic model, we have estimated the planet mass $M_2=17.9^{+9.6}_{-8.8}\,\mathrm{M}_\oplus$ and the lens distance $D_\mathrm{L}=6.7^{+1.0}_{-1.3}\,\mathrm{kpc}$, corresponding to a Neptune-mass planet close to the Galactic bulge. Such events with a low absolute latitude ($|b|\approx 1.1\,\mathrm{deg}$) are subject to both high extinction and more uncertain source distances, two factors that may affect the mass measurements in the provisional Wide Field Infrared Survey Telescope fields. More events are needed to investigate the potential trade-off between the higher lensing rate and the difficulty in measuring masses in these low-latitude fields., Comment: 30 pages, 8 figures, 5 tables. Typos corrected and section 3.2.3 added. Version accepted for publication in The Astronomical Journal
Published: 2018
Full Text: View/download PDF

46. OGLE-2014-BLG-0962 and the First Statistical Validation of Bayesian Priors for Galactic Microlensing

Author: Shan, Yutong, Yee, Jennifer C., Udalski, Andrzej, Bond, Ian A., Shvartzvald, Yossi, Shin, In-Gu, Jung, Youn-Kil, Novati, Sebastiano Calchi, Beichman, Charles A., Carey, Sean, Gaudi, B. Scott, Gould, Andrew, Pogge, Richard W., Poleski, Radosław, Skowron, Jan, Kozłowski, Szymon, Mróz, Przemysław, Pietrukowicz, Paweł, Szymański, Michał K., Soszyński, Igor, Ulaczyk, Krzysztof, Wyrzykowski, Łukasz, Abe, Fumio, Barry, Richard K., Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Maoz, Dan, Kaspi, Shai, Friedmann, Matan, Shan, Yutong, Yee, Jennifer C., Udalski, Andrzej, Bond, Ian A., Shvartzvald, Yossi, Shin, In-Gu, Jung, Youn-Kil, Novati, Sebastiano Calchi, Beichman, Charles A., Carey, Sean, Gaudi, B. Scott, Gould, Andrew, Pogge, Richard W., Poleski, Radosław, Skowron, Jan, Kozłowski, Szymon, Mróz, Przemysław, Pietrukowicz, Paweł, Szymański, Michał K., Soszyński, Igor, Ulaczyk, Krzysztof, Wyrzykowski, Łukasz, Abe, Fumio, Barry, Richard K., Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kawasaki, Kohei, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Maoz, Dan, Kaspi, Shai, and Friedmann, Matan
Abstract: OGLE-2014-BLG-0962 (OB140962) is a stellar binary microlensing event that was well-covered by observations from the Spitzer satellite as well as ground-based surveys. Modelling yields a unique physical solution: a mid-M+M-dwarf binary with $M_{\rm prim} = 0.20 \pm 0.01 M_\odot$ and $M_{\rm sec} = 0.16 \pm 0.01 M_\odot$, with projected separation of $2.0 \pm 0.3$ AU. The lens is only $D_{\rm LS} = 0.41 \pm 0.06$ kpc in front of the source, making OB140962 a bulge lens and the most distant Spitzer binary lens to date. In contrast, because the Einstein radius ($\theta_{\rm E} = 0.143 \pm 0.007$ mas) is unusually small, a standard Bayesian analysis, conducted in the absence of parallax information, would predict a brown dwarf binary. We test the accuracy of Bayesian analysis over a set of Spitzer lenses, finding overall good agreement throughout the sample. We also illustrate the methodology for probing the Galactic distribution of planets by comparing the cumulative distance distribution of the Spitzer 2-body lenses to that of the Spitzer single lenses., Comment: 15 pages, 7 figures, 5 tables; submitted to ApJ
Published: 2018

47. Continuum Reverberation Mapping of the Accretion Disks in Two Seyfert 1 Galaxies

Author: Fausnaugh, M. M., Starkey, D. A., Horne, Keith, Kochanek, C. S., Peterson, B. M., Bentz, M. C., Denney, K. D., Grier, C. J., Grupe, D., Pogge, R. W., DeRosa, G., Adams, S. M., Barth, A. J., Beatty, Thomas G., Bhattacharjee, A., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brown, Jacob E., Brown, Jonathan S., Brotherton, M. S., Coker, C. T., Crawford, S. M., Croxall, K. V., Eftekharzadeh, Sarah, Eracleous, Michael, Joner, M. D., Henderson, C. B., Holoien, T. W. -S., Hutchison, T., Kaspi, Shai, Kim, S., King, Anthea L., Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F., Manne-Nicholas, E. R., Mason, M., Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R., Nazarov, S. V., Nguyen, M. L., Okhmat, D. N., Onken, ChristopherA., Ou-Yang, B., Pancoast, A., Pei, L., Penny, Matthew T., Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E., Runnoe, Jessie, Sand, David J., Schimoia, Jaderson S., Sergeev, S. G., Shappee, B. J., Simonian, Gregory V., Somers, Garrett, Spencer, M., Stevens, Daniel J., Tayar, Jamie, Treu, T., Valenti, Stefano, VanSaders, J., VillanuevaJr., S., Villforth, C., Weiss, Yaniv, Winkler, H., Zhu, W., Fausnaugh, M. M., Starkey, D. A., Horne, Keith, Kochanek, C. S., Peterson, B. M., Bentz, M. C., Denney, K. D., Grier, C. J., Grupe, D., Pogge, R. W., DeRosa, G., Adams, S. M., Barth, A. J., Beatty, Thomas G., Bhattacharjee, A., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brown, Jacob E., Brown, Jonathan S., Brotherton, M. S., Coker, C. T., Crawford, S. M., Croxall, K. V., Eftekharzadeh, Sarah, Eracleous, Michael, Joner, M. D., Henderson, C. B., Holoien, T. W. -S., Hutchison, T., Kaspi, Shai, Kim, S., King, Anthea L., Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F., Manne-Nicholas, E. R., Mason, M., Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R., Nazarov, S. V., Nguyen, M. L., Okhmat, D. N., Onken, ChristopherA., Ou-Yang, B., Pancoast, A., Pei, L., Penny, Matthew T., Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E., Runnoe, Jessie, Sand, David J., Schimoia, Jaderson S., Sergeev, S. G., Shappee, B. J., Simonian, Gregory V., Somers, Garrett, Spencer, M., Stevens, Daniel J., Tayar, Jamie, Treu, T., Valenti, Stefano, VanSaders, J., VillanuevaJr., S., Villforth, C., Weiss, Yaniv, Winkler, H., and Zhu, W.
Abstract: We present optical continuum lags for two Seyfert 1 galaxies, MCG+08-11-011 and NGC 2617, using monitoring data from a reverberation mapping campaign carried out in 2014. Our light curves span the ugriz filters over four months, with median cadences of 1.0 and 0.6 days for MCG+08-11-011 and NGC\,2617, respectively, combined with roughly daily X-ray and near-UV data from Swift for NGC 2617. We find lags consistent with geometrically thin accretion-disk models that predict a lag-wavelength relation of $\tau \propto \lambda^{4/3}$. However, the observed lags are larger than predictions based on standard thin-disk theory by factors of 3.3 for MCG+08-11-011 and 2.3 for NGC\,2617. These differences can be explained if the mass accretion rates are larger than inferred from the optical luminosity by a factor of 4.3 in MCG+08-11-011 and a factor of 1.3 in NGC\,2617, although uncertainty in the SMBH masses determines the significance of this result. While the X-ray variability in NGC\,2617 precedes the UV/optical variability, the long 2.6 day lag is problematic for coronal reprocessing models., Comment: Accepted to ApJ, please send comments to faus@mit.edu. 24 pages, 8 figures
Published: 2018
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48. Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

Author: Blanton, Michael R., Bershady, Matthew A., Abolfathi, Bela, Albareti, Franco D., Prieto, Carlos Allende, Almeida, Andres, Alonso-García, Javier, Anders, Friedrich, Anderson, Scott F., Andrews, Brett, Aquino-Ortíz, Erik, Aragón-Salamanca, Alfonso, Argudo-Fernández, Maria, Armengaud, Eric, Aubourg, Eric, Avila-Reese, Vladimir, Badenes, Carles, Bailey, Stephen, Barger, Kathleen A., Barrera-Ballesteros, Jorge, Bartosz, Curtis, Bates, Dominic, Baumgarten, Falk, Bautista, Julian, Beaton, Rachael, Beers, Timothy C., Belfiore, Francesco, Bender, Chad F., Berlind, Andreas A., Bernardi, Mariangela, Beutler, Florian, Bird, Jonathan C., Bizyaev, Dmitry, Blanc, Guillermo A., Blomqvist, Michael, Bolton, Adam S., Boquien, Médéric, Borissova, Jura, Bosch, Remco van den, Bovy, Jo, Brandt, William N., Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burgasser, Adam J., Burtin, Etienne, Busca, Nicolás G., Cappellari, Michele, Carigi, Maria Leticia Delgado, Carlberg, Joleen K., Rosell, Aurelio Carnero, Carrera, Ricardo, Cherinka, Brian, Cheung, Edmond, Chew, Yilen Gómez Maqueo, Chiappini, Cristina, Choi, Peter Doohyun, Chojnowski, Drew, Chuang, Chia-Hsun, Chung, Haeun, Cirolini, Rafael Fernando, Clerc, Nicolas, Cohen, Roger E., Comparat, Johan, da Costa, Luiz, Cousinou, Marie-Claude, Covey, Kevin, Crane, Jeffrey D., Croft, Rupert A. C., Cruz-Gonzalez, Irene, Cuadra, Daniel Garrido, Cunha, Katia, Damke, Guillermo J., Darling, Jeremy, Davies, Roger, Dawson, Kyle, de la Macorra, Axel, De Lee, Nathan, Delubac, Timothée, Di Mille, Francesco, Diamond-Stanic, Aleks, Cano-Díaz, Mariana, Donor, John, Downes, Juan José, Drory, Niv, Bourboux, Hélion du Mas des, Duckworth, Christopher J., Dwelly, Tom, Dyer, Jamie, Ebelke, Garrett, Eisenstein, Daniel J., Emsellem, Eric, Eracleous, Mike, Escoffier, Stephanie, Evans, Michael L., Fan, Xiaohui, Fernández-Alvar, Emma, Fernandez-Trincado, J. G., Feuillet, Diane K., Finoguenov, Alexis, Fleming, Scott W., Font-Ribera, Andreu, Fredrickson, Alexander, Freischlad, Gordon, Frinchaboy, Peter M., Galbany, Lluís, Garcia-Dias, R., García-Hernández, D. A., Gaulme, Patrick, Geisler, Doug, Gelfand, Joseph D., Gil-Marín, Héctor, Gillespie, Bruce A., Goddard, Daniel, Gonzalez-Perez, Violeta, Grabowski, Kathleen, Green, Paul J., Grier, Catherine J., Gunn, James E., Guo, Hong, Guy, Julien, Hagen, Alex, Hahn, ChangHoon, Hall, Matthew, Harding, Paul, Hasselquist, Sten, Hawley, Suzanne L., Hearty, Fred, Hernández, Jonay I. Gonzalez, Ho, Shirley, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Holzer, Parker H., Huehnerhoff, Joseph, Hutchinson, Timothy A., Hwang, Ho Seong, Ibarra-Medel, Héctor J., Ilha, Gabriele da Silva, Ivans, Inese I., Ivory, KeShawn, Jackson, Kelly, Jensen, Trey W., Johnson, Jennifer A., Jones, Amy, Jönsson, Henrik, Jullo, Eric, Kamble, Vikrant, Kinemuchi, Karen, Kirkby, David, Kitaura, Francisco-Shu, Klaene, Mark, Knapp, Gillian R., Kneib, Jean-Paul, Kollmeier, Juna A., Lacerna, Ivan, Lane, Richard R., Lang, Dustin, Law, David R., Lazarz, Daniel, Goff, Jean-Marc Le, Liang, Fu-Heng, Li, Cheng, LI, Hongyu, Lima, Marcos, Lin, Lihwai, Lin, Yen-Ting, de Lis, Sara Bertran, Liu, Chao, Lizaola, Miguel Angel C. de Icaza, Long, Dan, Lucatello, Sara, Lundgren, Britt, MacDonald, Nicholas K., Machado, Alice Deconto, MacLeod, Chelsea L., Mahadevan, Suvrath, Maia, Marcio Antonio Geimba, Maiolino, Roberto, Majewski, Steven R., Malanushenko, Elena, Malanushenko, Viktor, Manchado, Arturo, Mao, Shude, Maraston, Claudia, Marques-Chaves, Rui, Masters, Karen L., McBride, Cameron K., McDermid, Richard M., McGrath, Brianne, McGreer, Ian D., Peña, Nicolás Medina, Melendez, Matthew, Merloni, Andrea, Merrifield, Michael R., Meszaros, Szabolcs, Meza, Andres, Minchev, Ivan, Minniti, Dante, Miyaji, Takamitsu, More, Surhud, Mulchaey, John, Müller-Sánchez, Francisco, Muna, Demitri, Munoz, Ricardo R., Myers, Adam D., Nair, Preethi, Nandra, Kirpal, Nascimento, Janaina Correa do, Negrete, Alenka, Ness, Melissa, Newman, Jeffrey A., Nichol, Robert C., Nidever, David L., Nitschelm, Christian, Ntelis, Pierros, O'Connell, Julia E., Oelkers, Ryan J., Oravetz, Audrey, Oravetz, Daniel, Pace, Zach, Padilla, Nelson, Palanque-Delabrouille, Nathalie, Palicio, Pedro Alonso, Pan, Kaike, Parikh, Taniya, Pâris, Isabelle, Park, Changbom, Patten, Alim Y., Peirani, Sebastien, Pellejero-Ibanez, Marcos, Penny, Samantha, Percival, Will J., Perez-Fournon, Ismael, Petitjean, Patrick, Pieri, Matthew M., Pinsonneault, Marc, Pisani, Alice, Poleski, Radosław, Prada, Francisco, Prakash, Abhishek, Queiroz, Anna Bárbara de Andrade, Raddick, M. Jordan, Raichoor, Anand, Rembold, Sandro Barboza, Richstein, Hannah, Riffel, Rogemar A., Riffel, Rogério, Rix, Hans-Walter, Robin, Annie C., Rockosi, Constance M., Rodríguez-Torres, Sergio, Roman-Lopes, A., Román-Zúñiga, Carlos, Rosado, Margarita, Ross, Ashley J., Rossi, Graziano, Ruan, John, Ruggeri, Rossana, Rykoff, Eli S., Salazar-Albornoz, Salvador, Salvato, Mara, Sánchez, Ariel G., Aguado, David Sánchez, Sánchez-Gallego, José R., Santana, Felipe A., Santiago, Basílio Xavier, Sayres, Conor, Schiavon, Ricardo P., Schimoia, Jaderson da Silva, Schlafly, Edward F., Schlegel, David J., Schneider, Donald P., Schultheis, Mathias, Schuster, William J., Schwope, Axel, Seo, Hee-Jong, Shao, Zhengyi, Shen, Shiyin, Shetrone, Matthew, Shull, Michael, Simon, Joshua D., Skinner, Danielle, Skrutskie, M. F., Slosar, Anže, Smith, Verne V., Sobeck, Jennifer S., Sobreira, Flavia, Somers, Garrett, Souto, Diogo, Stark, David V., Stassun, Keivan, Stauffer, Fritz, Steinmetz, Matthias, Storchi-Bergmann, Thaisa, Streblyanska, Alina, Stringfellow, Guy S., Suárez, Genaro, Sun, Jing, Suzuki, Nao, Szigeti, Laszlo, Taghizadeh-Popp, Manuchehr, Tang, Baitian, Tao, Charling, Tayar, Jamie, Tembe, Mita, Teske, Johanna, Thakar, Aniruddha R., Thomas, Daniel, Thompson, Benjamin A., Tinker, Jeremy L., Tissera, Patricia, Tojeiro, Rita, Toledo, Hector Hernandez, de la Torre, Sylvain, Tremonti, Christy, Troup, Nicholas W., Valenzuela, Octavio, Valpuesta, Inma Martinez, Vargas-González, Jaime, Vargas-Magaña, Mariana, Vazquez, Jose Alberto, Villanova, Sandro, Vivek, M., Vogt, Nicole, Wake, David, Walterbos, Rene, Wang, Yuting, Weaver, Benjamin Alan, Weijmans, Anne-Marie, Weinberg, David H., Westfall, Kyle B., Whelan, David G., Wild, Vivienne, Wilson, John, Wood-Vasey, W. M., Wylezalek, Dominika, Xiao, Ting, Yan, Renbin, Yang, Meng, Ybarra, Jason E., Yèche, Christophe, Zakamska, Nadia, Zamora, Olga, Zarrouk, Pauline, Zasowski, Gail, Zhang, Kai, Zhao, Gong-Bo, Zheng, Zheng, Zhou, Zhi-Min, Zhu, Guangtun B., Zoccali, Manuela, Zou, Hu, Blanton, Michael R., Bershady, Matthew A., Abolfathi, Bela, Albareti, Franco D., Prieto, Carlos Allende, Almeida, Andres, Alonso-García, Javier, Anders, Friedrich, Anderson, Scott F., Andrews, Brett, Aquino-Ortíz, Erik, Aragón-Salamanca, Alfonso, Argudo-Fernández, Maria, Armengaud, Eric, Aubourg, Eric, Avila-Reese, Vladimir, Badenes, Carles, Bailey, Stephen, Barger, Kathleen A., Barrera-Ballesteros, Jorge, Bartosz, Curtis, Bates, Dominic, Baumgarten, Falk, Bautista, Julian, Beaton, Rachael, Beers, Timothy C., Belfiore, Francesco, Bender, Chad F., Berlind, Andreas A., Bernardi, Mariangela, Beutler, Florian, Bird, Jonathan C., Bizyaev, Dmitry, Blanc, Guillermo A., Blomqvist, Michael, Bolton, Adam S., Boquien, Médéric, Borissova, Jura, Bosch, Remco van den, Bovy, Jo, Brandt, William N., Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burgasser, Adam J., Burtin, Etienne, Busca, Nicolás G., Cappellari, Michele, Carigi, Maria Leticia Delgado, Carlberg, Joleen K., Rosell, Aurelio Carnero, Carrera, Ricardo, Cherinka, Brian, Cheung, Edmond, Chew, Yilen Gómez Maqueo, Chiappini, Cristina, Choi, Peter Doohyun, Chojnowski, Drew, Chuang, Chia-Hsun, Chung, Haeun, Cirolini, Rafael Fernando, Clerc, Nicolas, Cohen, Roger E., Comparat, Johan, da Costa, Luiz, Cousinou, Marie-Claude, Covey, Kevin, Crane, Jeffrey D., Croft, Rupert A. C., Cruz-Gonzalez, Irene, Cuadra, Daniel Garrido, Cunha, Katia, Damke, Guillermo J., Darling, Jeremy, Davies, Roger, Dawson, Kyle, de la Macorra, Axel, De Lee, Nathan, Delubac, Timothée, Di Mille, Francesco, Diamond-Stanic, Aleks, Cano-Díaz, Mariana, Donor, John, Downes, Juan José, Drory, Niv, Bourboux, Hélion du Mas des, Duckworth, Christopher J., Dwelly, Tom, Dyer, Jamie, Ebelke, Garrett, Eisenstein, Daniel J., Emsellem, Eric, Eracleous, Mike, Escoffier, Stephanie, Evans, Michael L., Fan, Xiaohui, Fernández-Alvar, Emma, Fernandez-Trincado, J. G., Feuillet, Diane K., Finoguenov, Alexis, Fleming, Scott W., Font-Ribera, Andreu, Fredrickson, Alexander, Freischlad, Gordon, Frinchaboy, Peter M., Galbany, Lluís, Garcia-Dias, R., García-Hernández, D. A., Gaulme, Patrick, Geisler, Doug, Gelfand, Joseph D., Gil-Marín, Héctor, Gillespie, Bruce A., Goddard, Daniel, Gonzalez-Perez, Violeta, Grabowski, Kathleen, Green, Paul J., Grier, Catherine J., Gunn, James E., Guo, Hong, Guy, Julien, Hagen, Alex, Hahn, ChangHoon, Hall, Matthew, Harding, Paul, Hasselquist, Sten, Hawley, Suzanne L., Hearty, Fred, Hernández, Jonay I. Gonzalez, Ho, Shirley, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Holzer, Parker H., Huehnerhoff, Joseph, Hutchinson, Timothy A., Hwang, Ho Seong, Ibarra-Medel, Héctor J., Ilha, Gabriele da Silva, Ivans, Inese I., Ivory, KeShawn, Jackson, Kelly, Jensen, Trey W., Johnson, Jennifer A., Jones, Amy, Jönsson, Henrik, Jullo, Eric, Kamble, Vikrant, Kinemuchi, Karen, Kirkby, David, Kitaura, Francisco-Shu, Klaene, Mark, Knapp, Gillian R., Kneib, Jean-Paul, Kollmeier, Juna A., Lacerna, Ivan, Lane, Richard R., Lang, Dustin, Law, David R., Lazarz, Daniel, Goff, Jean-Marc Le, Liang, Fu-Heng, Li, Cheng, LI, Hongyu, Lima, Marcos, Lin, Lihwai, Lin, Yen-Ting, de Lis, Sara Bertran, Liu, Chao, Lizaola, Miguel Angel C. de Icaza, Long, Dan, Lucatello, Sara, Lundgren, Britt, MacDonald, Nicholas K., Machado, Alice Deconto, MacLeod, Chelsea L., Mahadevan, Suvrath, Maia, Marcio Antonio Geimba, Maiolino, Roberto, Majewski, Steven R., Malanushenko, Elena, Malanushenko, Viktor, Manchado, Arturo, Mao, Shude, Maraston, Claudia, Marques-Chaves, Rui, Masters, Karen L., McBride, Cameron K., McDermid, Richard M., McGrath, Brianne, McGreer, Ian D., Peña, Nicolás Medina, Melendez, Matthew, Merloni, Andrea, Merrifield, Michael R., Meszaros, Szabolcs, Meza, Andres, Minchev, Ivan, Minniti, Dante, Miyaji, Takamitsu, More, Surhud, Mulchaey, John, Müller-Sánchez, Francisco, Muna, Demitri, Munoz, Ricardo R., Myers, Adam D., Nair, Preethi, Nandra, Kirpal, Nascimento, Janaina Correa do, Negrete, Alenka, Ness, Melissa, Newman, Jeffrey A., Nichol, Robert C., Nidever, David L., Nitschelm, Christian, Ntelis, Pierros, O'Connell, Julia E., Oelkers, Ryan J., Oravetz, Audrey, Oravetz, Daniel, Pace, Zach, Padilla, Nelson, Palanque-Delabrouille, Nathalie, Palicio, Pedro Alonso, Pan, Kaike, Parikh, Taniya, Pâris, Isabelle, Park, Changbom, Patten, Alim Y., Peirani, Sebastien, Pellejero-Ibanez, Marcos, Penny, Samantha, Percival, Will J., Perez-Fournon, Ismael, Petitjean, Patrick, Pieri, Matthew M., Pinsonneault, Marc, Pisani, Alice, Poleski, Radosław, Prada, Francisco, Prakash, Abhishek, Queiroz, Anna Bárbara de Andrade, Raddick, M. Jordan, Raichoor, Anand, Rembold, Sandro Barboza, Richstein, Hannah, Riffel, Rogemar A., Riffel, Rogério, Rix, Hans-Walter, Robin, Annie C., Rockosi, Constance M., Rodríguez-Torres, Sergio, Roman-Lopes, A., Román-Zúñiga, Carlos, Rosado, Margarita, Ross, Ashley J., Rossi, Graziano, Ruan, John, Ruggeri, Rossana, Rykoff, Eli S., Salazar-Albornoz, Salvador, Salvato, Mara, Sánchez, Ariel G., Aguado, David Sánchez, Sánchez-Gallego, José R., Santana, Felipe A., Santiago, Basílio Xavier, Sayres, Conor, Schiavon, Ricardo P., Schimoia, Jaderson da Silva, Schlafly, Edward F., Schlegel, David J., Schneider, Donald P., Schultheis, Mathias, Schuster, William J., Schwope, Axel, Seo, Hee-Jong, Shao, Zhengyi, Shen, Shiyin, Shetrone, Matthew, Shull, Michael, Simon, Joshua D., Skinner, Danielle, Skrutskie, M. F., Slosar, Anže, Smith, Verne V., Sobeck, Jennifer S., Sobreira, Flavia, Somers, Garrett, Souto, Diogo, Stark, David V., Stassun, Keivan, Stauffer, Fritz, Steinmetz, Matthias, Storchi-Bergmann, Thaisa, Streblyanska, Alina, Stringfellow, Guy S., Suárez, Genaro, Sun, Jing, Suzuki, Nao, Szigeti, Laszlo, Taghizadeh-Popp, Manuchehr, Tang, Baitian, Tao, Charling, Tayar, Jamie, Tembe, Mita, Teske, Johanna, Thakar, Aniruddha R., Thomas, Daniel, Thompson, Benjamin A., Tinker, Jeremy L., Tissera, Patricia, Tojeiro, Rita, Toledo, Hector Hernandez, de la Torre, Sylvain, Tremonti, Christy, Troup, Nicholas W., Valenzuela, Octavio, Valpuesta, Inma Martinez, Vargas-González, Jaime, Vargas-Magaña, Mariana, Vazquez, Jose Alberto, Villanova, Sandro, Vivek, M., Vogt, Nicole, Wake, David, Walterbos, Rene, Wang, Yuting, Weaver, Benjamin Alan, Weijmans, Anne-Marie, Weinberg, David H., Westfall, Kyle B., Whelan, David G., Wild, Vivienne, Wilson, John, Wood-Vasey, W. M., Wylezalek, Dominika, Xiao, Ting, Yan, Renbin, Yang, Meng, Ybarra, Jason E., Yèche, Christophe, Zakamska, Nadia, Zamora, Olga, Zarrouk, Pauline, Zasowski, Gail, Zhang, Kai, Zhao, Gong-Bo, Zheng, Zheng, Zhou, Zhi-Min, Zhu, Guangtun B., Zoccali, Manuela, and Zou, Hu
Abstract: We describe the Sloan Digital Sky Survey IV (SDSS-IV), a project encompassing three major spectroscopic programs. The Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) is observing hundreds of thousands of Milky Way stars at high resolution and high signal-to-noise ratio in the near-infrared. The Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey is obtaining spatially-resolved spectroscopy for thousands of nearby galaxies (median redshift of z = 0.03). The extended Baryon Oscillation Spectroscopic Survey (eBOSS) is mapping the galaxy, quasar, and neutral gas distributions between redshifts z = 0.6 and 3.5 to constrain cosmology using baryon acoustic oscillations, redshift space distortions, and the shape of the power spectrum. Within eBOSS, we are conducting two major subprograms: the SPectroscopic IDentification of eROSITA Sources (SPIDERS), investigating X-ray AGN and galaxies in X-ray clusters, and the Time Domain Spectroscopic Survey (TDSS), obtaining spectra of variable sources. All programs use the 2.5-meter Sloan Foundation Telescope at Apache Point Observatory; observations there began in Summer 2014. APOGEE-2 also operates a second near-infrared spectrograph at the 2.5-meter du Pont Telescope at Las Campanas Observatory, with observations beginning in early 2017. Observations at both facilities are scheduled to continue through 2020. In keeping with previous SDSS policy, SDSS-IV provides regularly scheduled public data releases; the first one, Data Release 13, was made available in July 2016., Comment: Published in Astronomical Journal
Published: 2017
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49. Space Telescope and Optical Reverberation Mapping Project. V. Optical Spectroscopic Campaign and Emission-Line Analysis for NGC 5548

Author: Pei, L., Fausnaugh, M. M., Barth, A. J., Peterson, B. M., Bentz, M. C., De Rosa, G., Denney, K. D., Goad, M. R., Kochanek, C. S., Korista, K. T., Kriss, G. A., Pogge, R. W., Bennert, V. N., Brotherton, M., Clubb, K. I., Bontà, E. Dalla, Filippenko, A. V., Greene, J. E., Grier, C. J., Vestergaard, M., Zheng, W., Adams, Scott M., Beatty, Thomas G., Bigley, A., Brown, Jacob E., Brown, Jonathan S., Canalizo, G., Comerford, J. M., Coker, Carl T., Corsini, E. M., Croft, S., Croxall, K. V., Deason, A. J., Eracleous, Michael, Fox, O. D., Gates, E. L., Henderson, C. B., Holmbeck, E., Holoien, T. W. -S., Jensen, J. J., Johnson, C. A., Kelly, P. L., Kim, S., King, A., Lau, M. W., Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, Manne-Nicholas, E. R., Mauerhan, J. C., Malkan, M. A., McGurk, R., Morelli, L., Mosquera, Ana, Mudd, Dale, Sanchez, F. Muller, Nguyen, M. L., Ochner, P., Ou-Yang, B., Pancoast, A., Penny, Matthew T., Pizzella, A., Poleski, Radosław, Runnoe, Jessie, Scott, B., Schimoia, Jaderson S., Shappee, B. J., Shivvers, I., Simonian, Gregory V., Siviero, A., Somers, Garrett, Stevens, Daniel J., Strauss, M. A., Tayar, Jamie, Tejos, N., Treu, T., Van Saders, J., Vican, L., Villanueva Jr., S., Yuk, H., Zakamska, N. L., Zhu, W., Anderson, M. D., Arévalo, P., Bazhaw, C., Bisogni, S., Borman, G. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Cackett, E. M., Carini, M. T., Crenshaw, D. M., De Lorenzo-Cáceres, A., Dietrich, M., Edelson, R., Efimova, N. V., Ely, J., Evans, P. A., Ferland, G. J., Flatland, K., Gehrels, N., Geier, S., Gelbord, J. M., Grupe, D., Gupta, A., Hall, P. B., Hicks, S., Horenstein, D., Horne, Keith, Hutchison, T., Im, M., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Kim, M., Kim, S. C., Klimanov, S. A., Lee, J. C., Leonard, D. C., Lira, P., MacInnis, F., Mathur, S., McHardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Netzer, H., Norris, R. P., Nousek, J. A., Okhmat, D. N., Papadakis, I., Parks, J. R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Saylor, D. A., Schnülle, K., Sergeev, S. G., Siegel, M., Skielboe, A., Spencer, M., Starkey, D., Sung, H. -I., Teems, K. G., Turner, C. S., Uttley, P., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Zu, Y., Pei, L., Fausnaugh, M. M., Barth, A. J., Peterson, B. M., Bentz, M. C., De Rosa, G., Denney, K. D., Goad, M. R., Kochanek, C. S., Korista, K. T., Kriss, G. A., Pogge, R. W., Bennert, V. N., Brotherton, M., Clubb, K. I., Bontà, E. Dalla, Filippenko, A. V., Greene, J. E., Grier, C. J., Vestergaard, M., Zheng, W., Adams, Scott M., Beatty, Thomas G., Bigley, A., Brown, Jacob E., Brown, Jonathan S., Canalizo, G., Comerford, J. M., Coker, Carl T., Corsini, E. M., Croft, S., Croxall, K. V., Deason, A. J., Eracleous, Michael, Fox, O. D., Gates, E. L., Henderson, C. B., Holmbeck, E., Holoien, T. W. -S., Jensen, J. J., Johnson, C. A., Kelly, P. L., Kim, S., King, A., Lau, M. W., Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, Manne-Nicholas, E. R., Mauerhan, J. C., Malkan, M. A., McGurk, R., Morelli, L., Mosquera, Ana, Mudd, Dale, Sanchez, F. Muller, Nguyen, M. L., Ochner, P., Ou-Yang, B., Pancoast, A., Penny, Matthew T., Pizzella, A., Poleski, Radosław, Runnoe, Jessie, Scott, B., Schimoia, Jaderson S., Shappee, B. J., Shivvers, I., Simonian, Gregory V., Siviero, A., Somers, Garrett, Stevens, Daniel J., Strauss, M. A., Tayar, Jamie, Tejos, N., Treu, T., Van Saders, J., Vican, L., Villanueva Jr., S., Yuk, H., Zakamska, N. L., Zhu, W., Anderson, M. D., Arévalo, P., Bazhaw, C., Bisogni, S., Borman, G. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Cackett, E. M., Carini, M. T., Crenshaw, D. M., De Lorenzo-Cáceres, A., Dietrich, M., Edelson, R., Efimova, N. V., Ely, J., Evans, P. A., Ferland, G. J., Flatland, K., Gehrels, N., Geier, S., Gelbord, J. M., Grupe, D., Gupta, A., Hall, P. B., Hicks, S., Horenstein, D., Horne, Keith, Hutchison, T., Im, M., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Kim, M., Kim, S. C., Klimanov, S. A., Lee, J. C., Leonard, D. C., Lira, P., MacInnis, F., Mathur, S., McHardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Netzer, H., Norris, R. P., Nousek, J. A., Okhmat, D. N., Papadakis, I., Parks, J. R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Saylor, D. A., Schnülle, K., Sergeev, S. G., Siegel, M., Skielboe, A., Spencer, M., Starkey, D., Sung, H. -I., Teems, K. G., Turner, C. S., Uttley, P., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., and Zu, Y.
Abstract: We present the results of an optical spectroscopic monitoring program targeting NGC 5548 as part of a larger multi-wavelength reverberation mapping campaign. The campaign spanned six months and achieved an almost daily cadence with observations from five ground-based telescopes. The H$\beta$ and He II $\lambda$4686 broad emission-line light curves lag that of the 5100 $\AA$ optical continuum by $4.17^{+0.36}_{-0.36}$ days and $0.79^{+0.35}_{-0.34}$ days, respectively. The H$\beta$ lag relative to the 1158 $\AA$ ultraviolet continuum light curve measured by the Hubble Space Telescope is roughly $\sim$50% longer than that measured against the optical continuum, and the lag difference is consistent with the observed lag between the optical and ultraviolet continua. This suggests that the characteristic radius of the broad-line region is $\sim$50% larger than the value inferred from optical data alone. We also measured velocity-resolved emission-line lags for H$\beta$ and found a complex velocity-lag structure with shorter lags in the line wings, indicative of a broad-line region dominated by Keplerian motion. The responses of both the H$\beta$ and He II $\lambda$4686 emission lines to the driving continuum changed significantly halfway through the campaign, a phenomenon also observed for C IV, Ly $\alpha$, He II(+O III]), and Si IV(+O IV]) during the same monitoring period. Finally, given the optical luminosity of NGC 5548 during our campaign, the measured H$\beta$ lag is a factor of five shorter than the expected value implied by the $R_\mathrm{BLR} - L_\mathrm{AGN}$ relation based on the past behavior of NGC 5548., Comment: 22 pages, 13 figures, accepted to ApJ
Published: 2017
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50. Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

Author: Blanton, Michael R., Bershady, Matthew A., Abolfathi, Bela, Albareti, Franco D., Prieto, Carlos Allende, Almeida, Andres, Alonso-García, Javier, Anders, Friedrich, Anderson, Scott F., Andrews, Brett, Aquino-Ortíz, Erik, Aragón-Salamanca, Alfonso, Argudo-Fernández, Maria, Armengaud, Eric, Aubourg, Eric, Avila-Reese, Vladimir, Badenes, Carles, Bailey, Stephen, Barger, Kathleen A., Barrera-Ballesteros, Jorge, Bartosz, Curtis, Bates, Dominic, Baumgarten, Falk, Bautista, Julian, Beaton, Rachael, Beers, Timothy C., Belfiore, Francesco, Bender, Chad F., Berlind, Andreas A., Bernardi, Mariangela, Beutler, Florian, Bird, Jonathan C., Bizyaev, Dmitry, Blanc, Guillermo A., Blomqvist, Michael, Bolton, Adam S., Boquien, Médéric, Borissova, Jura, Bosch, Remco van den, Bovy, Jo, Brandt, William N., Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burgasser, Adam J., Burtin, Etienne, Busca, Nicolás G., Cappellari, Michele, Carigi, Maria Leticia Delgado, Carlberg, Joleen K., Rosell, Aurelio Carnero, Carrera, Ricardo, Cherinka, Brian, Cheung, Edmond, Chew, Yilen Gómez Maqueo, Chiappini, Cristina, Choi, Peter Doohyun, Chojnowski, Drew, Chuang, Chia-Hsun, Chung, Haeun, Cirolini, Rafael Fernando, Clerc, Nicolas, Cohen, Roger E., Comparat, Johan, da Costa, Luiz, Cousinou, Marie-Claude, Covey, Kevin, Crane, Jeffrey D., Croft, Rupert A. C., Cruz-Gonzalez, Irene, Cuadra, Daniel Garrido, Cunha, Katia, Damke, Guillermo J., Darling, Jeremy, Davies, Roger, Dawson, Kyle, de la Macorra, Axel, De Lee, Nathan, Delubac, Timothée, Di Mille, Francesco, Diamond-Stanic, Aleks, Cano-Díaz, Mariana, Donor, John, Downes, Juan José, Drory, Niv, Bourboux, Hélion du Mas des, Duckworth, Christopher J., Dwelly, Tom, Dyer, Jamie, Ebelke, Garrett, Eisenstein, Daniel J., Emsellem, Eric, Eracleous, Mike, Escoffier, Stephanie, Evans, Michael L., Fan, Xiaohui, Fernández-Alvar, Emma, Fernandez-Trincado, J. G., Feuillet, Diane K., Finoguenov, Alexis, Fleming, Scott W., Font-Ribera, Andreu, Fredrickson, Alexander, Freischlad, Gordon, Frinchaboy, Peter M., Galbany, Lluís, Garcia-Dias, R., García-Hernández, D. A., Gaulme, Patrick, Geisler, Doug, Gelfand, Joseph D., Gil-Marín, Héctor, Gillespie, Bruce A., Goddard, Daniel, Gonzalez-Perez, Violeta, Grabowski, Kathleen, Green, Paul J., Grier, Catherine J., Gunn, James E., Guo, Hong, Guy, Julien, Hagen, Alex, Hahn, ChangHoon, Hall, Matthew, Harding, Paul, Hasselquist, Sten, Hawley, Suzanne L., Hearty, Fred, Hernández, Jonay I. Gonzalez, Ho, Shirley, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Holzer, Parker H., Huehnerhoff, Joseph, Hutchinson, Timothy A., Hwang, Ho Seong, Ibarra-Medel, Héctor J., Ilha, Gabriele da Silva, Ivans, Inese I., Ivory, KeShawn, Jackson, Kelly, Jensen, Trey W., Johnson, Jennifer A., Jones, Amy, Jönsson, Henrik, Jullo, Eric, Kamble, Vikrant, Kinemuchi, Karen, Kirkby, David, Kitaura, Francisco-Shu, Klaene, Mark, Knapp, Gillian R., Kneib, Jean-Paul, Kollmeier, Juna A., Lacerna, Ivan, Lane, Richard R., Lang, Dustin, Law, David R., Lazarz, Daniel, Goff, Jean-Marc Le, Liang, Fu-Heng, Li, Cheng, LI, Hongyu, Lima, Marcos, Lin, Lihwai, Lin, Yen-Ting, de Lis, Sara Bertran, Liu, Chao, Lizaola, Miguel Angel C. de Icaza, Long, Dan, Lucatello, Sara, Lundgren, Britt, MacDonald, Nicholas K., Machado, Alice Deconto, MacLeod, Chelsea L., Mahadevan, Suvrath, Maia, Marcio Antonio Geimba, Maiolino, Roberto, Majewski, Steven R., Malanushenko, Elena, Malanushenko, Viktor, Manchado, Arturo, Mao, Shude, Maraston, Claudia, Marques-Chaves, Rui, Masters, Karen L., McBride, Cameron K., McDermid, Richard M., McGrath, Brianne, McGreer, Ian D., Peña, Nicolás Medina, Melendez, Matthew, Merloni, Andrea, Merrifield, Michael R., Meszaros, Szabolcs, Meza, Andres, Minchev, Ivan, Minniti, Dante, Miyaji, Takamitsu, More, Surhud, Mulchaey, John, Müller-Sánchez, Francisco, Muna, Demitri, Munoz, Ricardo R., Myers, Adam D., Nair, Preethi, Nandra, Kirpal, Nascimento, Janaina Correa do, Negrete, Alenka, Ness, Melissa, Newman, Jeffrey A., Nichol, Robert C., Nidever, David L., Nitschelm, Christian, Ntelis, Pierros, O'Connell, Julia E., Oelkers, Ryan J., Oravetz, Audrey, Oravetz, Daniel, Pace, Zach, Padilla, Nelson, Palanque-Delabrouille, Nathalie, Palicio, Pedro Alonso, Pan, Kaike, Parikh, Taniya, Pâris, Isabelle, Park, Changbom, Patten, Alim Y., Peirani, Sebastien, Pellejero-Ibanez, Marcos, Penny, Samantha, Percival, Will J., Perez-Fournon, Ismael, Petitjean, Patrick, Pieri, Matthew M., Pinsonneault, Marc, Pisani, Alice, Poleski, Radosław, Prada, Francisco, Prakash, Abhishek, Queiroz, Anna Bárbara de Andrade, Raddick, M. Jordan, Raichoor, Anand, Rembold, Sandro Barboza, Richstein, Hannah, Riffel, Rogemar A., Riffel, Rogério, Rix, Hans-Walter, Robin, Annie C., Rockosi, Constance M., Rodríguez-Torres, Sergio, Roman-Lopes, A., Román-Zúñiga, Carlos, Rosado, Margarita, Ross, Ashley J., Rossi, Graziano, Ruan, John, Ruggeri, Rossana, Rykoff, Eli S., Salazar-Albornoz, Salvador, Salvato, Mara, Sánchez, Ariel G., Aguado, David Sánchez, Sánchez-Gallego, José R., Santana, Felipe A., Santiago, Basílio Xavier, Sayres, Conor, Schiavon, Ricardo P., Schimoia, Jaderson da Silva, Schlafly, Edward F., Schlegel, David J., Schneider, Donald P., Schultheis, Mathias, Schuster, William J., Schwope, Axel, Seo, Hee-Jong, Shao, Zhengyi, Shen, Shiyin, Shetrone, Matthew, Shull, Michael, Simon, Joshua D., Skinner, Danielle, Skrutskie, M. F., Slosar, Anže, Smith, Verne V., Sobeck, Jennifer S., Sobreira, Flavia, Somers, Garrett, Souto, Diogo, Stark, David V., Stassun, Keivan, Stauffer, Fritz, Steinmetz, Matthias, Storchi-Bergmann, Thaisa, Streblyanska, Alina, Stringfellow, Guy S., Suárez, Genaro, Sun, Jing, Suzuki, Nao, Szigeti, Laszlo, Taghizadeh-Popp, Manuchehr, Tang, Baitian, Tao, Charling, Tayar, Jamie, Tembe, Mita, Teske, Johanna, Thakar, Aniruddha R., Thomas, Daniel, Thompson, Benjamin A., Tinker, Jeremy L., Tissera, Patricia, Tojeiro, Rita, Toledo, Hector Hernandez, de la Torre, Sylvain, Tremonti, Christy, Troup, Nicholas W., Valenzuela, Octavio, Valpuesta, Inma Martinez, Vargas-González, Jaime, Vargas-Magaña, Mariana, Vazquez, Jose Alberto, Villanova, Sandro, Vivek, M., Vogt, Nicole, Wake, David, Walterbos, Rene, Wang, Yuting, Weaver, Benjamin Alan, Weijmans, Anne-Marie, Weinberg, David H., Westfall, Kyle B., Whelan, David G., Wild, Vivienne, Wilson, John, Wood-Vasey, W. M., Wylezalek, Dominika, Xiao, Ting, Yan, Renbin, Yang, Meng, Ybarra, Jason E., Yèche, Christophe, Zakamska, Nadia, Zamora, Olga, Zarrouk, Pauline, Zasowski, Gail, Zhang, Kai, Zhao, Gong-Bo, Zheng, Zheng, Zhou, Zhi-Min, Zhu, Guangtun B., Zoccali, Manuela, Zou, Hu, Blanton, Michael R., Bershady, Matthew A., Abolfathi, Bela, Albareti, Franco D., Prieto, Carlos Allende, Almeida, Andres, Alonso-García, Javier, Anders, Friedrich, Anderson, Scott F., Andrews, Brett, Aquino-Ortíz, Erik, Aragón-Salamanca, Alfonso, Argudo-Fernández, Maria, Armengaud, Eric, Aubourg, Eric, Avila-Reese, Vladimir, Badenes, Carles, Bailey, Stephen, Barger, Kathleen A., Barrera-Ballesteros, Jorge, Bartosz, Curtis, Bates, Dominic, Baumgarten, Falk, Bautista, Julian, Beaton, Rachael, Beers, Timothy C., Belfiore, Francesco, Bender, Chad F., Berlind, Andreas A., Bernardi, Mariangela, Beutler, Florian, Bird, Jonathan C., Bizyaev, Dmitry, Blanc, Guillermo A., Blomqvist, Michael, Bolton, Adam S., Boquien, Médéric, Borissova, Jura, Bosch, Remco van den, Bovy, Jo, Brandt, William N., Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burgasser, Adam J., Burtin, Etienne, Busca, Nicolás G., Cappellari, Michele, Carigi, Maria Leticia Delgado, Carlberg, Joleen K., Rosell, Aurelio Carnero, Carrera, Ricardo, Cherinka, Brian, Cheung, Edmond, Chew, Yilen Gómez Maqueo, Chiappini, Cristina, Choi, Peter Doohyun, Chojnowski, Drew, Chuang, Chia-Hsun, Chung, Haeun, Cirolini, Rafael Fernando, Clerc, Nicolas, Cohen, Roger E., Comparat, Johan, da Costa, Luiz, Cousinou, Marie-Claude, Covey, Kevin, Crane, Jeffrey D., Croft, Rupert A. C., Cruz-Gonzalez, Irene, Cuadra, Daniel Garrido, Cunha, Katia, Damke, Guillermo J., Darling, Jeremy, Davies, Roger, Dawson, Kyle, de la Macorra, Axel, De Lee, Nathan, Delubac, Timothée, Di Mille, Francesco, Diamond-Stanic, Aleks, Cano-Díaz, Mariana, Donor, John, Downes, Juan José, Drory, Niv, Bourboux, Hélion du Mas des, Duckworth, Christopher J., Dwelly, Tom, Dyer, Jamie, Ebelke, Garrett, Eisenstein, Daniel J., Emsellem, Eric, Eracleous, Mike, Escoffier, Stephanie, Evans, Michael L., Fan, Xiaohui, Fernández-Alvar, Emma, Fernandez-Trincado, J. G., Feuillet, Diane K., Finoguenov, Alexis, Fleming, Scott W., Font-Ribera, Andreu, Fredrickson, Alexander, Freischlad, Gordon, Frinchaboy, Peter M., Galbany, Lluís, Garcia-Dias, R., García-Hernández, D. A., Gaulme, Patrick, Geisler, Doug, Gelfand, Joseph D., Gil-Marín, Héctor, Gillespie, Bruce A., Goddard, Daniel, Gonzalez-Perez, Violeta, Grabowski, Kathleen, Green, Paul J., Grier, Catherine J., Gunn, James E., Guo, Hong, Guy, Julien, Hagen, Alex, Hahn, ChangHoon, Hall, Matthew, Harding, Paul, Hasselquist, Sten, Hawley, Suzanne L., Hearty, Fred, Hernández, Jonay I. Gonzalez, Ho, Shirley, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Holzer, Parker H., Huehnerhoff, Joseph, Hutchinson, Timothy A., Hwang, Ho Seong, Ibarra-Medel, Héctor J., Ilha, Gabriele da Silva, Ivans, Inese I., Ivory, KeShawn, Jackson, Kelly, Jensen, Trey W., Johnson, Jennifer A., Jones, Amy, Jönsson, Henrik, Jullo, Eric, Kamble, Vikrant, Kinemuchi, Karen, Kirkby, David, Kitaura, Francisco-Shu, Klaene, Mark, Knapp, Gillian R., Kneib, Jean-Paul, Kollmeier, Juna A., Lacerna, Ivan, Lane, Richard R., Lang, Dustin, Law, David R., Lazarz, Daniel, Goff, Jean-Marc Le, Liang, Fu-Heng, Li, Cheng, LI, Hongyu, Lima, Marcos, Lin, Lihwai, Lin, Yen-Ting, de Lis, Sara Bertran, Liu, Chao, Lizaola, Miguel Angel C. de Icaza, Long, Dan, Lucatello, Sara, Lundgren, Britt, MacDonald, Nicholas K., Machado, Alice Deconto, MacLeod, Chelsea L., Mahadevan, Suvrath, Maia, Marcio Antonio Geimba, Maiolino, Roberto, Majewski, Steven R., Malanushenko, Elena, Malanushenko, Viktor, Manchado, Arturo, Mao, Shude, Maraston, Claudia, Marques-Chaves, Rui, Masters, Karen L., McBride, Cameron K., McDermid, Richard M., McGrath, Brianne, McGreer, Ian D., Peña, Nicolás Medina, Melendez, Matthew, Merloni, Andrea, Merrifield, Michael R., Meszaros, Szabolcs, Meza, Andres, Minchev, Ivan, Minniti, Dante, Miyaji, Takamitsu, More, Surhud, Mulchaey, John, Müller-Sánchez, Francisco, Muna, Demitri, Munoz, Ricardo R., Myers, Adam D., Nair, Preethi, Nandra, Kirpal, Nascimento, Janaina Correa do, Negrete, Alenka, Ness, Melissa, Newman, Jeffrey A., Nichol, Robert C., Nidever, David L., Nitschelm, Christian, Ntelis, Pierros, O'Connell, Julia E., Oelkers, Ryan J., Oravetz, Audrey, Oravetz, Daniel, Pace, Zach, Padilla, Nelson, Palanque-Delabrouille, Nathalie, Palicio, Pedro Alonso, Pan, Kaike, Parikh, Taniya, Pâris, Isabelle, Park, Changbom, Patten, Alim Y., Peirani, Sebastien, Pellejero-Ibanez, Marcos, Penny, Samantha, Percival, Will J., Perez-Fournon, Ismael, Petitjean, Patrick, Pieri, Matthew M., Pinsonneault, Marc, Pisani, Alice, Poleski, Radosław, Prada, Francisco, Prakash, Abhishek, Queiroz, Anna Bárbara de Andrade, Raddick, M. Jordan, Raichoor, Anand, Rembold, Sandro Barboza, Richstein, Hannah, Riffel, Rogemar A., Riffel, Rogério, Rix, Hans-Walter, Robin, Annie C., Rockosi, Constance M., Rodríguez-Torres, Sergio, Roman-Lopes, A., Román-Zúñiga, Carlos, Rosado, Margarita, Ross, Ashley J., Rossi, Graziano, Ruan, John, Ruggeri, Rossana, Rykoff, Eli S., Salazar-Albornoz, Salvador, Salvato, Mara, Sánchez, Ariel G., Aguado, David Sánchez, Sánchez-Gallego, José R., Santana, Felipe A., Santiago, Basílio Xavier, Sayres, Conor, Schiavon, Ricardo P., Schimoia, Jaderson da Silva, Schlafly, Edward F., Schlegel, David J., Schneider, Donald P., Schultheis, Mathias, Schuster, William J., Schwope, Axel, Seo, Hee-Jong, Shao, Zhengyi, Shen, Shiyin, Shetrone, Matthew, Shull, Michael, Simon, Joshua D., Skinner, Danielle, Skrutskie, M. F., Slosar, Anže, Smith, Verne V., Sobeck, Jennifer S., Sobreira, Flavia, Somers, Garrett, Souto, Diogo, Stark, David V., Stassun, Keivan, Stauffer, Fritz, Steinmetz, Matthias, Storchi-Bergmann, Thaisa, Streblyanska, Alina, Stringfellow, Guy S., Suárez, Genaro, Sun, Jing, Suzuki, Nao, Szigeti, Laszlo, Taghizadeh-Popp, Manuchehr, Tang, Baitian, Tao, Charling, Tayar, Jamie, Tembe, Mita, Teske, Johanna, Thakar, Aniruddha R., Thomas, Daniel, Thompson, Benjamin A., Tinker, Jeremy L., Tissera, Patricia, Tojeiro, Rita, Toledo, Hector Hernandez, de la Torre, Sylvain, Tremonti, Christy, Troup, Nicholas W., Valenzuela, Octavio, Valpuesta, Inma Martinez, Vargas-González, Jaime, Vargas-Magaña, Mariana, Vazquez, Jose Alberto, Villanova, Sandro, Vivek, M., Vogt, Nicole, Wake, David, Walterbos, Rene, Wang, Yuting, Weaver, Benjamin Alan, Weijmans, Anne-Marie, Weinberg, David H., Westfall, Kyle B., Whelan, David G., Wild, Vivienne, Wilson, John, Wood-Vasey, W. M., Wylezalek, Dominika, Xiao, Ting, Yan, Renbin, Yang, Meng, Ybarra, Jason E., Yèche, Christophe, Zakamska, Nadia, Zamora, Olga, Zarrouk, Pauline, Zasowski, Gail, Zhang, Kai, Zhao, Gong-Bo, Zheng, Zheng, Zhou, Zhi-Min, Zhu, Guangtun B., Zoccali, Manuela, and Zou, Hu
Abstract: We describe the Sloan Digital Sky Survey IV (SDSS-IV), a project encompassing three major spectroscopic programs. The Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) is observing hundreds of thousands of Milky Way stars at high resolution and high signal-to-noise ratio in the near-infrared. The Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey is obtaining spatially-resolved spectroscopy for thousands of nearby galaxies (median redshift of z = 0.03). The extended Baryon Oscillation Spectroscopic Survey (eBOSS) is mapping the galaxy, quasar, and neutral gas distributions between redshifts z = 0.6 and 3.5 to constrain cosmology using baryon acoustic oscillations, redshift space distortions, and the shape of the power spectrum. Within eBOSS, we are conducting two major subprograms: the SPectroscopic IDentification of eROSITA Sources (SPIDERS), investigating X-ray AGN and galaxies in X-ray clusters, and the Time Domain Spectroscopic Survey (TDSS), obtaining spectra of variable sources. All programs use the 2.5-meter Sloan Foundation Telescope at Apache Point Observatory; observations there began in Summer 2014. APOGEE-2 also operates a second near-infrared spectrograph at the 2.5-meter du Pont Telescope at Las Campanas Observatory, with observations beginning in early 2017. Observations at both facilities are scheduled to continue through 2020. In keeping with previous SDSS policy, SDSS-IV provides regularly scheduled public data releases; the first one, Data Release 13, was made available in July 2016., Comment: Published in Astronomical Journal
Published: 2017
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