adsabs/AstroCLIMB huggingface dataset:
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Top: a 3 × 3 postage stamp plot where the top left panel is the observed density plot NGC 5897, and the other panels are example noise maps generated to assess the significance of the excess in NGC 5897, as described in Section 3.1. Note that regions masked in white correspond to pixels with values equal to 0 in the raw data, corresponding to a lack of coverage (see Figure 3). The red and yellow circles correspond to rt and rJ, respectively, and the colorscale corresponds to what is shown in Figure 3. Bottom: An azimuthally averaged density profile of the background-subtracted observed data is shown as blue points, with the mean, 1σ, and 2σ of the distribution of density profiles from 1000 noise map samples shown in black/gray. The observed excess at the rJ is at a 4.6σ significance relative to distribution of density profiles from the noise maps.
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Same as Figure 2, but for NGC 7492. A clear photometric excess is seen beyond the Jacobi radius of the GC (yellow circle). As with NGC 5897, this excess does not preferentially align with the proper motion of NGC 7492 (red arrow).
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Same as Figure 5, but for NGC 7492. The significance of the observed excess just beyond the Jacobi radius is 2.8σ, while being 1.9σ at the Jacobi radius.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: The upper panels: integrated [O III]λ5007 contours at [3, 15, 40, 80, 105] × σ (where σ = 6.2 × 10−19 erg s−1 cm−2) overlaid on the images of the same integrated [O III]λ5007 line emission image in the left, the [O III]λ5007 emission-line velocity field (moment 1) in the middle, and the velocity dispersion (moment 2) in the right. The lower panels: integrated Hβ contours at [3, 7, 15, 25] × σ (where σ = 6.0 × 10−19 erg s−1 cm−2) overlaid on the images of the same integrated Hβ line emission image in the left, the Hβ emission-line velocity field (moment 1) in the middle, and the velocity dispersion (moment 2) in the right. The images in velocity fields (moment 1) and the velocity dispersions (moment 2) are generated by those spaxels above 3σch, where σch is the mean channel noise (σch = 5.4 × 10−19 erg s−1 cm−2 Å−1). The black cross represents the same the center of integrated Hα image with Figure 1. The black line is the major axis of Hα image with PA = 25°. The PA of the white-dashed line is 46°. The oval in the lower left corner represents the spatial resolution ﹩2\mathop{.}\limits^{^{\prime\prime} }5\times 1\mathop{.}\limits^{^{\prime\prime} }3﹩.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Left panel: Hα to Hβ flux ratio within 3σ Hβ region. The red contours (integrated [O III]λ5007 at [3, 15, 40, 80, 105] × σ, where σ = 6.2 × 10−19 erg s−1 cm−2) are the same as [O III]λ5007 contours in Figures 5, 6, and 8. The resolution of integrated Hα and Hβ images have been convolved to the same value (﹩2\mathop{.}\limits^{^{\prime\prime} }5﹩ × ﹩1\mathop{.}\limits^{^{\prime\prime} }5﹩). Right panel: the absolute value of equivalent width (∣EW∣) of [O III]λ5007. The figure is masked by Hβ 3σ region for better comparison with Hα to Hβ flux ratio. The red contours are the same as the left panel. The ∣EW∣ is in the unit of Å.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: BPT diagram. The blue dots represent each spaxel of AGC 111629 within 3σ [N II]λ6583 and Hβ region as show in Figure 10(b). The red dots with errors represent the center peanut-shaped structure within [O III]λ5007 40σ region (see Figure 8). The typical error is the mean value of all blue dots. Gray dots represent galaxies from the MPA-JHU SDSS DR7 (J. Brinchmann et al. 2004). The gray solid line is from L. J. Kewley et al. (2001), the dotted line is from G. Kauffmann et al. (2003a), and the dashed line is from K. Schawinski et al. (2007). The model data points (purple, green, dark orange, and brown squares) are from M. S. Polimera et al. (2022) for a low-metallicity theoretical dwarf galaxy with a continuous star-formation history, a metallicity of Z = 0.4Z⊙, and a 0%, 8%, 16%, or 100% AGN contribution to its spectrum from a black hole with MBH = 105.0 M⊙.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Integrated Hα contours at [3, 8, 18, 36] × σ (where σ = 8.3 × 10−19 erg s−1 cm−2) are overlaid on the integrated [N II] line emission image in panel (a) and on the gas-phase abundance maps of 12+log(O/H) in panels (b) and (c). The metallicity in panel (b) is derived using only spaxels with [N II] detections above 3σ[NII] (1 σ[NII] = 7.0 × 10−19 erg s−1 cm−2), while panel (c) includes spaxels with lower signal-to-noise ratios. The oval in the lower left corner represents the spatial resolution ﹩2\mathop{.}\limits^{^{\prime\prime} }5\times 1\mathop{.}\limits^{^{\prime\prime} }1﹩.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: [O III]λ5007 to Hβ flux ratio within 3σ Hβ region. The blue contours (integrated [O III]λ5007 at [3, 15, 40, 80, 105] × σ, where σ = 6.2 × 10−19 erg s−1 cm−2) are the same as [O III]λ5007 contours in Figures 5 and 6.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Integrated [O III]λ5007 emission contours (white lines) at [3, 15, 40, 80, 105] × σ (where σ = 6.2 × 10−19 erg s−1 cm−2) overlaid on DESI g-band image (in the left panel) and integrated Hα image (in the right panel) of AGC 111629. The red square is the same region of Figure 5.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: The red line is the H I spectrum from ALFALFA, and the blue dots represent the integrated Hα spectrum of AGC 111629 among the 3σ contour region in Figure 1(a). The blue solid line is the Gaussian fitting of the integrated Hα spectrum. The gray dashed line is the systemic velocity of the Gaussian fitting center 6457 km s−1 which is consistent with the center of H I spectrum 6454 km s−1.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Integrated Hα emission contours (white lines) at [3, 8, 18, 36] × σ (where σ = 8.3 × 10−19 erg s−1 cm−2) overlaid on DESI g-band image of AGC 111629. The point source near AGC 111629 is identified as a star in SDSS. The red square is the same region of Figure 1.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Left panel: the Hα PVD along the major axis of AGC 111629. Hα is shown in gray with blue contours. Right panel: The Hα PVD along the minor axis of AGC 111629. The red line marks the arch-like structure position in Figure 1(b). 1″ corresponds to 0.43 kpc.