adsabs/AstroCLIMB huggingface dataset:
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Galaxy luminosity function (left), MUV–Mh relation (middle), and star formation efficiency (﹩\mathrm{SFR}/{\dot{M}}_{{\rm{h}}}\mbox{--}{M}_{{\rm{h}}}﹩ relation, right) in cases of the DPL and Schechter luminosity functions. The blue, orange, magenta, and pink solid (dashed) lines represent relations in the case of the DPL (Schechter) luminosity functions at z ∼ 4, 6, 8, and 10, respectively. To reproduce the observed bright-end excess of the number density like the DPL function (the solid line in the left panel), the higher star formation efficiency (the solid line in the right panel) is needed at the massive end, compared to the case of the Schechter function (the dashed line). The blue and orange symbols in the middle panel show the results of this study (diamonds), Harikane et al. (2018a; crosses), and Harikane et al. (2016; circles). In the right panel, the black solid curve is the fitting formulae of Equation (56), and the gray shaded region represents the 2σ typical scatter (0.3 dex).
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Distribution of SC candidates in the Galactic coordinate system. New clusters mean the 61 newly identified clusters with relatively clear CMDs, while uncertified candidates denote those without clear CMDs within newly identified candidates. Matched clusters mean that the known clusters that have been found by previous works.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Differential reddening distribution of 61 newly identified clusters with relatively clear CMDs. The unit of differential reddening is mag.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Comparison of best-fit and observed CMDs of nine newly identified SCs with clear main sequences. Black points are for observed stars, and red triangles are for best-fit stellar populations. The name of each cluster in the LISC catalog and its possible SPT are given in the figure.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Similar to Figure 3, but for 12 other newly identified clusters.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Similar to Figure 3, but for 20 other newly identified clusters.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Age (i.e., in the figure) distribution of 61 newly identified clusters. For CSPs, the age of the youngest stars is taken. The unit of age is gigayears.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Metallicity (Z) distribution of 61 newly identified clusters.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Primordial binary fraction (fbin) distribution of 61 newly identified clusters.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Comparison of observed and best-fit CMDs of some example known SCs. All SCs have eMSTO structures, and their SPTs seem to be CSPs.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Similar to Figure 10, but for 20 other known SCs with eMSTO structures, and their SPTs seem to be SSPs.
Paper: LISC Catalog of Star Clusters. I. Galactic Disk Clusters in Gaia EDR3
Authors: Zhongmu Li, Yangyang Deng, Huanbin Chi, Jing Chen, Xuejie Liu, Chen Yan, Wen Chen, Wenkai Guo, and Tao Xia
Figure caption: Similar to Figure 10, but for 20 other known SCs. The SPTs of these clusters seem to be SSPs.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Discovery spectra of the first set of 16 quasars, displayed in decreasing order of redshift. The object name and the estimated redshift (with uncertainty Δz ∼ 0.01–0.1; see text) are indicated in the upper left corner of each panel, with the two asterisks indicating that the object is noted in the text. The five type II quasar candidates are marked with “TII” adjacent to the redshifts. The blue dotted lines mark the expected positions of the Lyα and N V λ1240 emission lines, given the redshifts. The spectra were smoothed using inverse-variance-weighted means over 3–13 pixels (depending on the S/N), for display purposes. The bottom panel displays a sky spectrum, as a guide to the expected noise.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Same as Figure 1, but for the second set of 16 quasars.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Same as Figure 1, but for the third set of 16 quasars.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Same as Figure 1, but for the fourth set of 16 quasars.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Same as Figure 1, but for the last set of quasars in the top five panels. The following panels present seven galaxies and an [O III] emitter, with the expected positions of Si II λ1260, Si II λ1304, and C II λ1335 (for the galaxies) and of Hγ, Hβ, and [O III] λλ4959, 5007 lines (for the [O III] emitter) marked by the dotted lines.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Same as Figure 1, but for the first set of 16 Galactic cool stars and brown dwarfs, ordered by the R.A. The red lines represent the best-fit templates, whose spectral types are indicated in the upper left corner of the individual panels.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Same as Figure 6, but for the last set of 15 Galactic dwarfs.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Median-stacked spectra of the high-z objects discovered by SHELLQs. The top three panels present those created from 51 quasars with M1450 < −24.2, 49 quasars with −23.5 < M1450 < −24.2, and 39 quasars with M1450 > −23.5, while the bottom panel presents that created from 38 galaxies. The median M1450 of the stacked objects is reported in each panel.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Redshifts and the rest-frame ultraviolet absolute magnitudes (M1450) of all the high-z objects reported in the past and present SHELLQs papers, including quasars (blue circles), type II quasar candidates (blue circles enclosed by larger circles), and galaxies (green circles). We also plot all the other high-z quasars published to date (gray circles), compiled mostly from the papers referenced in Section 1.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: Examples of the transmitted fluxes in the GP trough, found along the sight lines toward J021430.90+023240.4 (top) and J021847.04+000715.0 (bottom). The black and cyan lines represent the observed fluxes and associated 1σ errors, respectively.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Nobunari Kashikawa, Michael A. Strauss, Masatoshi Imanishi, Tohru Nagao, Masayuki Akiyama, John D. Silverman, Naoko Asami, James Bosch, Hisanori Furusawa, Tomotsugu Goto, James E. Gunn, Yuichi Harikane, Hiroyuki Ikeda, Rikako Ishimoto, Toshihiro Kawaguchi, Nanako Kato, Satoshi Kikuta, Kotaro Kohno, Yutaka Komiyama, Chien-Hsiu Lee, Robert H. Lupton, Takeo Minezaki, Satoshi Miyazaki, Hitoshi Murayama, Atsushi J. Nishizawa, Masamune Oguri, Yoshiaki Ono, Masami Ouchi, Paul A. Price, Hiroaki Sameshima, Naoshi Sugiyama, Philip J. Tait, Masahiro Takada, Ayumi Takahashi, Tadafumi Takata, Masayuki Tanaka, Yoshiki Toba, Yousuke Utsumi, Shiang-Yu Wang, and Takuji Yamashita
Figure caption: HSC i − z and z − y colors of the high-z quasars (blue symbols), the high-z galaxies (green), the [O III] emitters at z = 0.8–1.0 (cyan), and Galactic cool stars and brown dwarfs (red), with spectroscopic identification reported in the past and present SHELLQs papers; the filled and open circles represent those with ﹩{P}_{Q}^{B}\gt 0.1﹩ and ﹩{P}_{Q}^{B}\leqslant 0.1﹩, respectively. The magnitudes are taken from PDR3. The arrows represent 3σ limits, while the objects detected only in the y band are placed at ﹩{i}_{\mathrm{AB}}-{z}_{\mathrm{AB}}={i}_{\mathrm{AB}}^{\mathrm{lim}}-{z}_{\mathrm{AB}}^{\mathrm{lim}}﹩ with dotted error bars, where ﹩{m}_{\mathrm{AB}}^{\mathrm{lim}}﹩ represents the 3σ limiting magnitude. We also plot the model colors of quasars (solid curve) and galaxies (dashed curve) at z ≥ 5.7, with the diamonds marking redshifts at Δz = 0.1 intervals. The gray plus signs and circles represent simulated colors of main-sequence stars and M-, L-, and T-type brown dwarfs, as indicated in the lower left corner (see Matsuoka et al. 2016, for the details of those models). The hatched area represents the color cuts used in Step 1 of the selection (see Section 2).
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Examples of phase-folded light curves of HBSs from our collection. Here and throughout the paper, the orbital phase equal to 1.0 corresponds to the periastron passage, and P denotes the orbital period.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Phase-folded light curves of the sample of OGLE HBSs with different shapes. The orbital inclination, i, and the argument of the periastron, ω, were obtained by fitting Kumar et al.’s model to the phase-folded light curves. In the rows, we present HBSs with i equal to circa 40°, 60°, and 80°, respectively. The obtained ω parameter increases horizontally from 0° to 180°. The HBSs with ω equal to about 0° or 180° during the heartbeat show two minima and one maximum of brightness, while for ω ≈ 90° we can see two maxima and one minimum. With increasing i parameter, the minima become deeper. Note, that the right- and left-hand sides in this figure are almost symmetrical reflections of each other.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Shape of the HBS light curve as a function of eccentricity, e. We used the phase-folded and normalized light curves of the OGLE HBSs. The light curves are shifted in magnitude to avoid overlaps. The e parameter (numbers on the right-hand side) were obtained using Kumar et al.’s model. For low eccentric orbits, the light curves have sinusoidal-like shapes, similar to the classical ellipsoidal variables (top). With increasing e, the phase range of the heartbeat becomes narrower (bottom). For e ≈ 0.8, the duration of the heartbeat is about 10% of the orbital period.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Distribution of the HBSs in the sky toward the GB (left panel) and in the MCs (right panel). Black contours correspond to the OGLE-IV footprint. Dotted and dashed black lines denote the galactic and equatorial coordinates, respectively. The blue and red points represent the OGLE ellipsoidal variables and HBSs, respectively. Note that the HBSs from the LMC align along the central bar.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Histograms of basic observational and orbital parameters of the HBSs located toward the GB (red boxes) and in the MCs (blue boxes). With the solid black line, we denote a histogram of the combined samples of the HBSs from all locations. In the panels, we present histograms of (a) the mean I-band magnitude; (b) the mean V-band magnitude; (c) V − I color index; (d) orbital period, P; (e) I-band peak-to-peak amplitude (based on the fitted model of Kumar et al.), A; (f) orbital eccentricity, e.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Examples of phase-folded light curves of the eclipsing HBSs from our collection.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Phase-folded light curves (left panels) and a close-up view on the heartbeat (part of the phase-folded light curve between dashed red lines; right panels) of six eclipsing HBSs, where the eclipse appears very close to the minimum brightness of the heartbeat.