adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The difference between broadband color computed in our catalog compared to ASTRODEEP, for the cluster (top) and parallel (bottom) parts of the MACSJ0416 field. The colors and symbols are the same as those in Figure 10.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: WISE 3.4 μm images of our sample galaxies (north is up and east is to the left). A bar on the upper right corner in each panel indicates 1 kpc. The integer in the brackets after the galaxy name indicates the detection (1) or nondetection (0) of the ALMA CO observation. FCC 117 and PGC 012625 are not clearly detected in the WISE band.
Paper: New Methanol Maser Transitions and Maser Variability Identified from an Accretion Burst Source G358.93-0.03
Authors: Dan Miao, Xi Chen, Shi-Min Song, Andrej M. Sobolev, Shari L. Breen, Gordon C. MacLeod, Bin Li, Sergey Parfenov, Anastasia Bisyarina, Zhi-Qiang Shen
Figure caption: Spectra of previously known CH3OH and H2O maser transitions monitored over a period of 2 months associated with G358.93-0.03. Information on the molecule, transition, and frequency are given at the upper left of each panel and the dates are given at the upper right, similar to Figure 1. The spectra observed on different dates are shown in different colors.
Paper: New Methanol Maser Transitions and Maser Variability Identified from an Accretion Burst Source G358.93-0.03
Authors: Dan Miao, Xi Chen, Shi-Min Song, Andrej M. Sobolev, Shari L. Breen, Gordon C. MacLeod, Bin Li, Sergey Parfenov, Anastasia Bisyarina, Zhi-Qiang Shen
Figure caption: Spectra of the eight new CH3OH maser transitions detected from G358.93-0.03 with the TMRT. Transitions and frequencies are given at the upper left of each panel and the date is given as a number MDD (where “M” stands for month and “DD” stands for day) at the upper right. The 26.12 GHz transition is shown with spectra observed at all five epochs. For the remaining new transitions, those observed with the wideband mode in April are shown with red lines, and those observed with the zoom-band mode in May are shown with black lines. Note that both the 31.98 GHz and 46.56 GHz transitions were not detected with the zoom-band mode in 2019 May.
Paper: New Methanol Maser Transitions and Maser Variability Identified from an Accretion Burst Source G358.93-0.03
Authors: Dan Miao, Xi Chen, Shi-Min Song, Andrej M. Sobolev, Shari L. Breen, Gordon C. MacLeod, Bin Li, Sergey Parfenov, Anastasia Bisyarina, Zhi-Qiang Shen
Figure caption: Rotation diagram for the eight new detected methanol transitions. Different colors represent different transitions. The frequencies and dates (for example, 503 represents 2019 May 3) of the spectral lines are marked on the upper right. The five points in the upper-left corner were observed in May and the other three points in the lower-right corner were observed in April.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Comparison between the Fornax galaxies and field galaxies from the z0MGS (Leroy et al. 2019), xGASS (Catinella et al. 2018), and xCOLDGASS (Saintonge et al. 2017) projects: M star dependences of (a) SFR, (b) sSFR, (c) ﹩{R}_{{{\rm{H}}}_{2}}={M}_{{{\rm{H}}}_{2}}/{M}_{{\rm{H}}\,{\rm\small{I}}}﹩, (d) μ gas = M gas/M star, (e) μ H I = M H I/M star, (f) ﹩{\mu }_{{{\rm{H}}}_{2}}={M}_{{{\rm{H}}}_{2}}/{M}_{\mathrm{star}}﹩, (g) SFEgas = SFR/M gas, (h) SFEH I = SFR/M H I, (i) SFE﹩{}_{{{\rm{H}}}_{2}}﹩ = SFR/﹩{M}_{{{\rm{H}}}_{2}}﹩. The main sequence of star-forming galaxies defined in Speagle et al. (2014) is indicated as purple dotted lines, and the 0.2 dex scatter range is indicated as purple shading in panels (a) and (b). The field relations are estimated with CO- or H I–detected galaxies, i.e., star-forming galaxies, and indicated as dashed (with nonparametric fitting) and solid (with third-order polynomial fitting) lines in panels (c)–(i). Gray-shaded regions are the errors of the nonparametric fitting and estimated by the bootstrap method with a 95% confidence interval. The Fornax galaxies with CO/H I detection and nondetection are indicated as blue filled circles/orange filled squares and blue open circles/orange open squares, respectively. The contours indicate field star-forming galaxies used to derive the field relations. The lower/upper limits of the field galaxies are indicated as open triangles/inverted triangles. In panels (d) and (g), ﹩{M}_{{{\rm{H}}}_{2}}/{M}_{\mathrm{star}}﹩ and SFR/﹩{M}_{{{\rm{H}}}_{2}}﹩ are plotted for the galaxies without H I data, respectively. For the ﹩{R}_{{{\rm{H}}}_{2}}﹩ panel, the field galaxies with H I and CO upper limits are indicated as X marks.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Radial variation of key quantities whose M star dependence has been subtracted, i.e., Δ(Field) values. The black filled circle and its upper/lower limits indicate the median and first/third quartiles, respectively. The individual data are indicated as gray filled circles. Zero of each key quantity indicates the values of the field galaxies (dashed line), and the gray-shaded regions indicate the 1σ of the Δ(Field) values for the field galaxies. Note that the numbers of galaxies used to plot in each panel are different. The Spearman’s rank-order correlation coefficient r and the p-value are shown on the lower left corner of each panel in purple. Only ﹩{\rm{\Delta }}(\mathrm{Field}),{\mu }_{{{\rm{H}}}_{2}}﹩ significantly correlates to the clustocentric distance.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: H I–H2 comparison of the offsets from the field SF galaxies at fixed stellar masses of gas fraction (a) and SFE (b). The galaxies with both CO and H I detection are indicated as circles, and those with upper limits are indicated as arrows. The color of the symbol indicates Δ(MS). The contours indicate the field galaxies with CO and H I detection. The Spearman’s rank-order correlation coefficient r and the p-value are shown on the lower left corner of each panel in purple. Although there is no clear correlation between Δ(Field), μ H I, and ﹩{\rm{\Delta }}(\mathrm{Field}),{\mu }_{{{\rm{H}}}_{2}}﹩ or Δ(Field), SFEH I, and ﹩{\rm{\Delta }}(\mathrm{Field}),{\mathrm{SFE}}_{{{\rm{H}}}_{2}}﹩, our Fornax sample with H I and H2 measurements tends to be more depleted in H I than in H2 and tends to have higher SFEH I than field galaxies, whereas their SFE﹩{}_{{{\rm{H}}}_{2}}﹩ is comparable to that of the field galaxies.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Comparison between the Fornax galaxies and field galaxies with M star > 109 M ⊙: relationships between the offsets from the main sequence of star-forming galaxies [Δ(MS) = Δ(Field)SFR] with Δ(Field) values of gas fractions, ﹩{R}_{{{\rm{H}}}_{2}}﹩, and SFEs. The contours indicate field galaxies with CO/H I detection, and filled black circles indicate the Fornax galaxies with CO/H I detection. The Spearman’s rank-order correlation coefficient r and the p-value are shown on the lower left corner of each panel in purple. Our Fornax sample has lower gas fractions and higher ﹩{R}_{{{\rm{H}}}_{2}}﹩ and SFEs than the field galaxies at Δ(MS) ∼ −1.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Comparison between the Fornax galaxies (solid line) and field galaxies (dashed line) with M star > 109 M ⊙: histograms for the offsets from the field relations, Δ(Field). Note that Δ(Field)s of SFR and sSFR are calculated based on the SFMS definition in Speagle et al. (2014). The medians for the Fornax and field galaxies are indicated at the upper left corner. The p-value for the K-S test comparing the Fornax and field galaxies is indicated at the upper right corner. Our Fornax sample has lower SFR, sSFR, and gas fractions and higher ﹩{R}_{{{\rm{H}}}_{2}}﹩, SFEgas, and SFEH I for their masses. SFE﹩{}_{{{\rm{H}}}_{2}}﹩ of our Fornax sample is not significantly different from the one of the field galaxies.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption:  M mol comparison between Zabel et al. (2019) (M mol,12M) and this study (M mol,ACA). The Spearman’s correlation coefficient and its p-value are presented at the upper left corner in purple. The galaxies with a large M mol value tend to have a high M mol,ACA/M mol,12M ratio, suggesting the missing flux in the 12 m data.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: (a) Δ(Field)SFR, (b) ﹩{\rm{\Delta }}{(\mathrm{Field})}_{{\mu }_{{{\rm{H}}}_{2}}}﹩, and (c) ﹩{\rm{\Delta }}{(\mathrm{Field})}_{{\mathrm{SFE}}_{{{\rm{H}}}_{2}}}﹩ on the PSD. The gray contours indicate the FCC galaxies with the NED velocity (NASA/IPAC Extragalactic Database 2019). The triangle region enclosed by the solid black line is the VIR region. The boundary for the RPS region is indicated with the dotted line and is too close to the y-axis of the plot to be recognized in this plot. The rest of the region is the RIF region. The CO nondetections are indicated with triangles.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: The relationships between R 5,sky with the key quantities [Δ(Field) values]. Symbols are the same as in Figure 10. R 5,sky positively correlates to SFR, sSFR, μ gas, and ﹩{\mu }_{{{\rm{H}}}_{2}}﹩ and negatively correlates to ﹩{R}_{{{\rm{H}}}_{2}}﹩.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Comparison of M star and SFR estimations in Leroy et al. (2019) (M star,z0MGS and SFRz0MGS) and the ones in this study (M star,CAAPR and SFRCAAPR).
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Ancillary images and CO moment maps of ESO 358-51: (a) WISE 3.4 μm, (b) GALEX FUV, (c) WISE 22 μm, (d) CO integrated-intensity map, (e) CO velocity map, and (f) CO velocity-dispersion map. The CO spectrum is also shown in panel (d). The vertical and horizontal axes of the CO spectrum plot are the brightness temperatures in units of millikelvin and the velocity in units of kilometers per second, respectively. The black and gray dotted lines on the CO spectrum panel indicate the galaxy systemic velocity and the velocity range in which the molecular gas mass is calculated, respectively. The red and gray contours indicate CO integrated-intensity maps. The aperture ellipse for the WISE and GALEX data to calculate M star and SFR is indicated with a white solid line. The magenta line indicates the area to generate total CO spectra (shown in panel (d)) to calculate M mol.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Relationship between the accretion phase, (∣Δv gal∣/σ Fornax) × (R proj/R 200), with the key quantities. Symbols are the same as in Figure 10. Among all the environmental parameters, SFR, sSFR, and ﹩{\mu }_{{{\rm{H}}}_{2}}﹩ most strongly depend on the accretion phase, where ancient infallers tend to have lower SFR, sSFR, and ﹩{\mu }_{{{\rm{H}}}_{2}}﹩ values than the recent infallers.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for IC 1993.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for ESO 358-G063.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for MCG-06-08-024.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for MCG-06-09-023.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for NGC 1310.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for ESO 359-2.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Same as Figure 14, but for FCC 332.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: Cumulative histograms of stellar mass and the key quantities of galaxies in the VIR (solid line) and RIF (dashed line). The numbers of galaxies in the VIR and RIF regions are indicated at the upper left corner in each panel. The p-values of the K-S test are indicated in purple at the lower right corner.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: PSD of our sample galaxies in the Fornax cluster, color-coded for the key quantities defined in Section 4.
Paper: Optical Variability of Eight FRII-type Quasars with 13 yr Photometric Light Curves
Authors: Agnieszka Kuźmicz, Arti Goyal, Stanisław Zola, Marek Jamrozy, Marek Dróżdż, Waldemar Ogłoza, Michał Siwak, Daniel E. Reichart, Vladimir V. Kouprianov, Daniel B. Caton
Figure caption: Top to bottom: (Left) R-band light curves for B2 0709+37, FBQS J095206.3+235245, PG 1004+130, [HB89] 1156+631, [HB89] 1425+267, [HB89] 1503+691, [HB89] 1721+343, and 4C +74.268 quasars. The quasar variability is expressed as the relative magnitude changes with respect to the comparison star. In the bottom part of each graph, we plot the relative magnitudes between the comparison and the check star. (Right) Corresponding SFs (Section 4.1). For large time lags Δt (gray points), the sampling of the SF is poor due to the finite range of the time series, and the characteristic plateau is not visible. Therefore, we do not take them into account when fitting the four-parameter SF function plotted in red. The red point corresponds to the decorrelation timescale τ (Equation (2)).
Paper: Optical Variability of Eight FRII-type Quasars with 13 yr Photometric Light Curves
Authors: Agnieszka Kuźmicz, Arti Goyal, Stanisław Zola, Marek Jamrozy, Marek Dróżdż, Waldemar Ogłoza, Michał Siwak, Daniel E. Reichart, Vladimir V. Kouprianov, Daniel B. Caton
Figure caption: Radio–optical overlaps of the observed quasars. The 1.4 GHz NRAO Very Large Array Sky Survey (NVSS; Condon et al. 1998) black contours are overlaid onto the r-band Pan-STARRS optical images. The 1.4 GHz Faint Images of the Radio Sky at Twenty-Centimeters (FIRST; Becker et al. 1995) radio contours are plotted in red, and the 3 GHz Very Large Array Sky Survey (VLASS; Lacy et al. 2020) contours are in magenta. The contour levels start at nominal 3σ rms noise levels of 1.35, 0.6, and 0.12 mJy beam−1 for the NVSS, FIRST, and VLASS surveys, respectively, and increase by factors of ﹩{\left(\sqrt{2}\right)}^{n}﹩ where n ranges from 0, 1, 2, 3... . The crosses mark the position of the parent QSO.
Paper: Optical Variability of Eight FRII-type Quasars with 13 yr Photometric Light Curves
Authors: Agnieszka Kuźmicz, Arti Goyal, Stanisław Zola, Marek Jamrozy, Marek Dróżdż, Waldemar Ogłoza, Michał Siwak, Daniel E. Reichart, Vladimir V. Kouprianov, Daniel B. Caton
Figure caption: Best-fit PSDs and the corresponding p  β  curves for our quasar light curves. The dashed line shows the raw periodogram while the blue triangles and red circles give the logarithmically binned power spectrum and the best-fit power spectrum, respectively. The error on the best-fit PSD slope corresponds to a 68% confidence limit, derived from fitting a Gaussian function to the p  β  curve and is given as standard deviation, σ. The dashed horizontal line corresponds to the statistical noise floor level due to measurement noise.
Paper: Optical Variability of Eight FRII-type Quasars with 13 yr Photometric Light Curves
Authors: Agnieszka Kuźmicz, Arti Goyal, Stanisław Zola, Marek Jamrozy, Marek Dróżdż, Waldemar Ogłoza, Michał Siwak, Daniel E. Reichart, Vladimir V. Kouprianov, Daniel B. Caton
Figure caption: SFs for B2 0709+37. The black points show the SF derived from the original light curve, while the red points show the SF derived from the evenly sampled light curve obtained by interpolation of the observed one.