adsabs/AstroCLIMB huggingface dataset:
Paper: CO Observations of Early-mid Stage Major Mergers in the MaNGA Survey
Authors: Qingzheng Yu, 清正 余, Taotao Fang, 陶陶 方, Cong Kevin Xu, 聪 徐, Shuai Feng, 帅 冯, Siyi Feng, 思轶 冯, Yu Gao, 煜 高, Xue-Jian Jiang, 雪健 蒋, Ute Lisenfeld
Figure caption: (a) ΔSFR as a function of ﹩{\rm{\Delta }}{f}_{{{\rm{H}}}_{2}}﹩. (b) ΔSFR as a function of ﹩{\rm{\Delta }}{M}_{{{\rm{H}}}_{2}}﹩/M H I . Paired galaxies at different merger stages and the control sample are marked with blue, orange, red, and black, respectively. In each plot, the Spearman coefficients of the relations in each subsample are labeled in the southeast corner.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Experiment III: reconstructions results of the galaxy cluster PSZ2 G165.68+44.01. The first and third rows show the ground-truth image and the estimated images obtained by the imaging algorithms (logarithmic scale). The second and fourth rows show the dirty image and the corresponding residual dirty images (linear scale). For R3D3, we showcase the results of its realization with J = 6 layers in its R2D2-Net components. Values of (S/N, log S/N) are reported below estimated images. The ﹩{\overline{\sigma }}_{{\rm{res.}}}﹩ values are indicated below the residual dirty images.
Paper: The R2D2 Deep Neural Network Series Paradigm for Fast Precision Imaging in Radio Astronomy
Authors: Amir Aghabiglou, Chung San Chu, Arwa Dabbech, Yves Wiaux
Figure caption: Experiment IV: reconstructions results of the radio galaxy Messier 106. The first and third rows show the ground-truth image and the estimated images obtained by the imaging algorithms (logarithmic scale). The second and fourth rows show the dirty image and the corresponding residual dirty images (linear scale). For R3D3, we showcase the results of its realization with J = 6 layers in its R2D2-Net components. Values of (S/N, log S/N) are reported below estimated images. The ﹩{\overline{\sigma }}_{{\rm{res.}}}﹩ values are indicated below the residual dirty images.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: BUFFALO cluster footprints analyzed in this work. The HST mosaics were calibrated, aligned, and created following the approaches described in Koekemoer et al. (2011), and the BUFFALO data set is described in Steinhardt et al. (2020). The RGB color pictures were created using trilogy (Coe et al. 2012), using F160W as the red channel, F105W as the green channel, and F814W as the blue channel. Note that due to the larger area coverage of F814W (ACS) compared to other bands (WFC3), certain areas of the footprint appear as blue. In the top-left panel, we include the JWST NIRSpec apertures for reference. We also include the most recent HFF-image footprint for each cluster in red.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Representative examples of the point-spread function (PSF) for the instruments used in this study, corresponding to a 0.″06 pixel−1 scale normalized with the ZScale algorithm. From left to right, panels show ACS-F814W (inner region), ACS-F814W (outer region), WFC3-F160W (inner region), WFC3-F160W (outer region). See Section 3.1 for more details.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Assessing the quality of photometric redshifts estimated through SED fitting. Top panel: photometric vs. spectroscopic redshift comparison. Blue and orange points are 709 matched BUFFALO and HFF sources, respectively, selected to have a BUFFALO F160W-band magnitude between 16 and 26, detected in at least five BUFFALO bands, and with a redshift quality flag >3. The solid line shows the 1:1 relationship, and the dashed lines encloses the z phot = z spec ± 0.15(1 + z spec) threshold used to identify outliers (i.e., catastrophic errors). NMAD scatter (σ) and outlier fraction (η) are reported on the top-left corner. Bottom panel: Δz ≡ z phot − z spec scatter. We include the ±0.15 dashed lines to denote the outlier boundary.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Assessing the quality of photometric redshifts estimated through SED fitting. Top panel: photometric vs. spectroscopic redshift comparison. Blue points are 999 spectroscopic redshifts selected for 16 < F160W < 26, detected in at least five bands, with a redshift quality flag >3. The solid line shows the 1:1 relationship and the dashed lines encloses the z phot = z spec ± 0.15 (1 + z spec) threshold used to identify outliers (i.e., catastrophic errors). The median of Δz/(1 + z spec) (bias) and outlier fraction (η) are reported on the top-left corner. Bottom panel: Δz ≡ z phot − z spec scatter.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Photometric validation of the BUFFALO catalogs. Scatterplot of Δmag = magin − magout as a function of the input magnitude for the different bands considered in this work. Each one of the blue points corresponds to a different recovered injected source. The solid line shows the rolling mean magnitude offset and the shaded area corresponds to the interquartile range. A broken horizontal dark line at 0, and at gray lines at  ±50 mmag are also added to each panel as visual aids. Additionally, each panel includes the input magnitude histogram (top horizontal histogram) as well as the Δmag histogram (right vertical histogram).
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Steps in bright cluster + ICL modeling (in this case for cluster MACS-1149) for the F160W band. Upper panels show the original image (left) and the galaxy/ICL models (right). Lower panels show the residual image before and after median filtering (left- and right-hand panel respectively). The color bar denotes the pixel intensity in counts per second. See Sections 3.2–3.3 for more details.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Top panel: comparison of magnitude distribution in the F160W band between BUFFALO sources (solid lines) and HFF (broken lines) for both the cluster and parallel (par) fields in the deepest part of the images for MACS J1149. Bottom panel: ratio between the histograms in the top panel for the cluster field (blue open circles) and parallel field (orange crosses). Other fields show similar behavior.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Empirical correction to the reported SEXTRACTOR errors using synthetic sources for Ks (top), I1 (middle), and I2 (bottom) bands. The error ratio is the ratio between the standard deviation of the magnitude residuals of the injected sources in a given magnitude bin, and the median reported error by T-PHOT. Error bars are computed via bootstrap resampling. The best-fit power-law model for each band is shown as orange lines.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Magnitude comparison between “hot+cold” mode as described in P21, and the “super hot” mode used in this work. Note, the magnitude difference is primarily within 0.05 mag.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Redshift histograms for each cluster field. Dotted lines correspond to the redshift of the cluster. Sources were chosen with magABF160W < 28.5 and χ 2/ndof < 5.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Magnitude distributions for sources in the BUFFALO catalogs across all clusters. We subdivide each of the catalogs, one per cluster and per parallel/infall field, into inner (in) and outer (out) regions, which correspond to different depth regimes.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption:                         The main sequence (MS) of star-forming galaxies. We represent each galaxy of the PHANGS-HST sample as a U − B vs. V − I color–color diagram (Figure 12) at the position on the MS of their host galaxy. The color–color diagrams are presented by contours computed for the ML catalog of C1 and C2 clusters. As a reference, we show for each diagram the BC03-model track in red. For crowded regions, we shift the color–color diagrams and denote their position on the MS with a red point and an arrow. For those galaxies that are not in a crowded region, we mark their position on the MS with a red star, situated in the center of the color–color diagrams. The purple background represents the density of SDSS galaxies of z < 0.2 with M                   * and SFR values computed by Salim et al. (2016). The dashed line is the predicted MS at z = 0 defined by Leroy et al. (2021), and the gray area shows the standard deviation computed by Catinella et al. (2018). The essence of this figure is the connection between star formation activity and the cluster population of all PHANGS-HST galaxies. As discussed in the text, the star formation rates are sensitive to timescales of <100 Myr, and therefore, the relative fractions of MAP clusters correlate with the relative position on the MS as shown in Figure 14.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Number fraction of C1 and C2 clusters of each galaxy associated with the main characteristic regions in color–color diagrams found in Section 4.4 as a function of ΔMS. We show the YCL, the MAP, and the OGC in blue, green, and red, respectively. In gray, we show clusters outside the main regions. We distinguish galaxies at a distance of smaller and larger than 15 Mpc with full and open circles respectively. For each panel, we show the Pearson correlation coefficient in the top right. Since the MAP shows a strong correlation, which we explain in the text, we fitted a linear function to the data points and provide the fit parameters.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Characteristic regions in U − B vs. V − I color–color diagrams of C1 and C2 clusters and C3 compact associations. We show human- and ML-classified samples in the top and bottom row, respectively. We compute the color–color maps by stacking each cluster as a normalized Gaussian function on a grid using the color uncertainties as standard deviations. We then identify the YCL (blue) and the MAP (green) as the contour lines encircling 50% of the highest point for C1 clusters and C3 compact associations, respectively. We then find the largest contour line, which only encircles the OGC (red), separating this region from the MAP. We show the hulls of all three regions for C2 clusters. In order to compare the slope of the reddening vector and the sequence of dust-reddened objects in the YCL, we fit a linear function to all C3 compact association, which are inside the blue segmented area.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: UBVI color–color diagrams for each individual PHANGS-HST galaxies. We present ML-classified class 1 and 2 clusters with black contours. With green and blue points, we overplot human-classified class 1 and 2 clusters, respectively. For reference, we show the solar metallicity track with a red line of the BC03 model. To indicate the direction of color–color shift due to reddening, we show a black arrow in the top left, which indicates a reddening of A  V  = 1. To study the color–color distribution of each galaxy with respect to the position of the main sequence (MS) of star-forming galaxies (see Figure 13), we sort the diagrams in decreasing order of ΔMS values.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Number fraction of C1 and C2 clusters of each galaxy associated with the main characteristic regions in color–color diagrams found in Section 4.4 as a function of galaxy distance. We show the YCL, the MAP, and the OGC in blue, green, and red, respectively. In gray, we show clusters outside the main regions. We distinguish distance measurements that are estimated from stellar markers such as tip of the red giant branch or from Cepheid variable stars, marked with full circles, whereas other distant measurements are less precise and are marked by empty circles. A complete discussion on each individual distance measurement is provided in Anand et al. (2020) and Anand et al. (2021). For each panel, we show the Pearson correlation coefficient in the top right.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Color–color diagram of ML-classified class 1 and 2 clusters in three bins of stellar mass. The most massive clusters with M * > 104 M ⊙ are shown in the left panel, intermediate masses of 5 × 103 M ⊙ > M * < 104 M ⊙ are in the middle panel, and low-mass clusters of M * < 5 × 103 M ⊙ are in the right panel. Similar to Figure 6, we use a density heat map to illustrate the distribution of clusters.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Histograms representing the percentage of C1 + C2 compact clusters associated with molecular clouds. We show for each characteristic region (YCL, MAP, and OGCC) the percentages of clusters that are cospatial with ALMA CO(2-1) molecular gas detection with an S/N > 6. The human-classified and machine-learning-classified samples are shown separately.
Paper: PHANGS-HST Catalogs for ∼100,000 Star Clusters and Compact Associations in 38 Galaxies. I. Observed Properties
Authors: Daniel Maschmann, Janice C. Lee, David A. Thilker, Bradley C. Whitmore, Sinan Deger, Médéric Boquien, Rupali Chandar, Daniel A. Dale, Aida Wofford, Stephen Hannon, Kirsten L. Larson, Adam K. Leroy, Eva Schinnerer, Erik Rosolowsky, Leonardo Úbeda, Ashley T. Barnes, Eric Emsellem, Kathryn Grasha, Brent Groves, Rémy Indebetouw, Hwihyun Kim, Ralf S. Klessen, Kathryn Kreckel, Rebecca C. Levy, Francesca Pinna, M. Jimena Rodríguez, Qiushi Tian, Thomas G. Williams
Figure caption: Same as Figure 10 but with NUV-B colors on the y-axis.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: The figure shows a multiwavelength overlay images of GRQs and GRGs. SDSS/Pan-STARRS r-band optical images are overlaid with TGSS (purple contours), LoTSS-DR2 (yellow contours), FIRST (blue contours), and VLASS (where first coverage is not available; red contours) images. For all images, contours are overplotted with 10 levels spaced in log scale with the lowest level of 3σ. The black cursor mark represents the position of the host counterpart.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: All-sky projection of the distribution of newly discovered GRS in the sky is shown with red circles. We also added GRS from four large samples, namely Dabhade et al. (2020c; in green), Andernach et al. (2021; in cyan), Kuźmicz & Jamrozy (2021; in gray), and Kuźmicz et al. (2018; in crimson).
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: This figure shows a zoomed-in plot of the optical spectrum of the host of a GRQ (J0804+2722) obtained from SDSS. Gaussians are fitted to Hβ and [O III] doublet spectral lines. The broadness of Hβ line is a clear indication of its quasar nature. The blue line represents the observed spectra, and the red line represents the best-fitted spectra.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: This plot depicts the optical spectrum of an HEGRG (J1512+4541) using SDSS. The observed spectra is represented by the blue line, whereas the best-fitted spectra is denoted by the red line.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: WISE color–color plot with the TGSS GRS sample is shown. This plot also includes 1007 sources from the previous GRG catalogs along with our newly discovered 34 GRSs. Here, 237 sources are from Kuźmicz et al. (2018), 137 sources are from Dabhade et al. (2020c), 242 GRSs are from Dabhade et al. (2020b), 165 are from Andernach et al. (2021), 170 GRQs are from Kuźmicz & Jamrozy (2021), and 56 radio sources are from Simonte et al. (2022).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)