adsabs/AstroCLIMB huggingface dataset:
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: (a) The velocity width–diameter relation, (b) diameter–mass relation, (c) velocity width–mass relation, and (d) virial ratio–mass relation for starless cores in Orion A. The best-fit lines for bounded cores, unbounded cores, and all starless cores are shown in (a), (b), and (c). The red and blue dots are the bound and unbound cores, respectively. The dashed line in (d) at ﹩{\alpha }_{\mathrm{vir}}={M}_{\mathrm{vir}}/{M}_{\mathrm{core}}=2﹩ shows the boundary between bound and unbound cores.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The core diameter–mass relation in four areas. The dotted lines denote the relation of ﹩{M}_{\mathrm{core}}\propto {(2{R}_{\mathrm{core}})}^{3}﹩. The red and blue dots are the bound (α vir ≤ 2) and unbound (α vir > 2) cores, respectively. The red dashed line in panel (a) is a best-fit function for low-mass (<1 M ⊙) bound starless cores.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of core diameters for unbound starless cores (red), bound starless cores (blue), and protostellar cores (dashed line) in the four subregions: (a) OMC-1/2/3, (b) OMC-4/5, (c) L1641N/V380 Ori, and (d) L1641C, respectively.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of core masses for unbound starless cores (red), bound starless cores (blue), and protostellar cores (dashed line) in the four subregions. Each panel is for the same area as in Figure 10.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of virial ratios for unbound starless cores (red), bound starless cores (blue), and protostellar cores (dashed line) for the four subregions. Each panel is for the same area as in Figure 10.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The velocity width–diameter relation in four subregions.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of FWHM velocity widths for unbound starless cores (red), bound starless cores (blue), and protostellar cores (dashed line) in the four subregions. Each panel is for the same area as in Figure 10.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of densities for unbound starless cores (red), bound starless cores (blue), and protostellar cores (dashed line) for the four subregions. Each panel is for the same area as in Figure 10.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of core aspect ratios for unbound starless cores (red), bound starless cores (blue), and protostellar cores (dashed line) in the four subregions. Each panel is for the same area as in Figure 10.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The core lifetime vs. core density for four areas. The solid lines show t ff and 10t ff. The dashed lines are best-fit functions from the second-lowest density points (﹩{n}_{\mathrm{core}}\,\sim ﹩ 103 cm−3) to the ends in the form of a power-law function. The shaded area in each panel indicates the area with the lifetime is between 5t ff and 30t ff. The error bar in each panel just represents the statistical uncertainty calculated with the square root of the number of cores of each plot, ﹩\sqrt{N}﹩; other uncertainties such as the number of class II objects are not included.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The virial ratio–mass relation in four subregions. The horizontal dashed lines indicate α vir = 2.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The core decl. vs. the central velocity relation for four areas. The four panels correspond to the same area of Figure 10. The vertical axis in each panel is the decl. in the offset from ﹩-5^\circ 30^{\prime} ﹩ in units of arcminutes. The bound starless cores, unbound starless cores, and protostellar cores are represented as filled red circles, open blue circles, and orange squares, respectively.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The velocity width–mass relation in four subregions. The red dashed line in panel (a) represents a best-fit function for low-mass (<1 M ⊙) bound starless cores as well as in Figure 18.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The core lifetime vs. core density in Orion A. Details are the same as for Figure 23.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same figure as Figure 25 but for the core decl. vs. the velocity width in the FWHM relation.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The freefall times of starless cores as a function of core masses in Orion A.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same figure as Figure 25 but for the core decl. vs. the core mass relation.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same as Figure 21 but for four subregions in Orion A. Each panel is for the same area as in Figure 10.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: (a) The observed CMFs for all cores (magenta), all starless cores (green), and bound starless cores (red) in the whole Orion A area. The error bars show the statistical uncertainty calculated as the square root of the number of cores in each mass bin, ﹩\sqrt{N}﹩. The dotted lines show the best-fit power-law functions for each CMF between two mass bins above the turnover and the high-mass end. The detection mass limit is estimated to be 0.016 M ⊙. (b) Comparison between the CMF of bounded starless cores (red) and the stellar IMF in the ONC region (blue). Their distributions look very similar, and the peak masses are comparable to each other. The vertical dashed lines in both panels are the completeness limits.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: CMF for bound starless cores (red) and the expected CMF with core growth by mass accretion (blue). We assumed that ﹩1\ {M}_{\mathrm{core}}﹩ gas accretes on the ﹩1\ {M}_{\mathrm{core}}﹩ core within a certain time and calculated the mass accretion rate for each core.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same as Figure 29, left. Panels (a)–(d) show the CMFs in areas (a)–(d), respectively, delineated in Figure 1. Details are the same as for Figure 29.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same as Figure 30, but starless cores with virial ratios of unity or less are classified as bound cores. Details are the same as for Figure 29.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same as Figure 23, but starless cores with virial ratios of unity or less are classified as bound cores. Details are the same as for Figure 24.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same figure as Figure 25 but for the core decl. vs. the density relation.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: The 6′ × 6′ black squares show the nine large boxes adopted to sample the background. The mean background value in counts per pixel estimated for the central box is shown in red. The numbers corresponding to other boxes (in blue) convey the measured percentage difference of the local background mean (i.e., measured within each box) from the estimated mean of the central box in one random run as explained in Section 2.2. The error value associated with the background flux within a 6′ × 6′ box is ∼0.24%. The region outlined by the red dashed rectangle indicates the HST coverage. The black dashed circle, which has a radius of 13′ from the UVIT field center, shows the area for which we provide the catalog. This figure highlights the relative variation in the FUV background across the UVIT field.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: The distribution of the sky background as measured with 3600 random boxes (400 within each large box shown in Figure 4), each having a size of 11 × 11 pixels in the UVIT images in F154W (left), N242W (middle), and N245M (right). The optimal SExtractor detection thresholds adopted for F154W, N242W, and N245M filters are 1.25σ, 1.15σ, and 1.50σ respectively. The histogram for the optimal threshold in each respective filter is shown in blue solid line, while the distributions for the other two thresholds are displayed (to show the variation in skewness) in gray dashed and dotted lines. For the optimal detection threshold, the plotted distribution shows one among the 100 random iterations performed to estimate the global background values listed in Table 3.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: False color composite image of the GOODS-N field observed by AstroSat/UVIT. The background shows a part of the full UVIT circular field of diameter 28′. The blue, red, and green colors represent emission in F154W, N242W, and N245M filters respectively. The white polygon shows the HST coverage as observed in CANDELS (Grogin et al. 2011; Koekemoer et al. 2011). The catalog presented in this work includes sources detected within 13′ from the UVIT field center (as shown in Figure 4).
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: Effective area profile of the three UVIT filters used for observation (data obtained from Tandon et al. 2020). The y-axis also shows the value of percentage throughput.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: Flowchart showing the data processing steps for producing UVIT Level (2) images from the raw Level (1) data using the CCDLAB software (Postma & Leahy 2017). The calibration data for FPN noise, distortion, and flat-fielding are obtained from the UVIT calibration database. Details of the data reduction procedure using CCDLAB are given in Postma & Leahy (2021).
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: The distribution of the background rms as measured within the same 3600 random boxes of Figure 5 for the same choice of SExtractor parameter values for UVIT F154W (left), N242W (middle), and N245M (right). Here, also, each distribution is one of 100 random iterations.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: The empirical PSFs in three UVIT filters. The NUV PSFs are constructed by stacking the images of 10 stars identified in the UVIT field, whereas we find only 2 candidate stars in the FUV. The panel insets show the core of each PSF.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: Differential number count (number/deg2/0.5 mag) histograms vs. AB magnitude of sources detected within ﹩13^{\prime} ﹩ from the UVIT field center (i.e., within the black dashed circle shown in Figure 4) for F154W (top), N242W (middle), and N245M (bottom). All source photometry used circular apertures with a radius of 1.″4, and was corrected using the aperture correction derived from the PSF for that filter. The mean (﹩\overline{m}﹩) and median (﹩\widetilde{m}﹩) values of each distribution are noted in the figure. The red and blue dashed lines mark the 3σ detection and 50% completeness limit, respectively. The photometry in the N245M band was performed in dual-mode using the N242W band image as the detection image, whereas the F154W and N242W source detections and photometry were performed in those images individually.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: Left: the FWHM of 10 selected stars in N242W bands are plotted with their distance from the field center. The adjacent histogram shows the distribution of measured FWHM of the selected stars. The error bar plotted on the top left shows the typical error in the estimated FWHM. Right: the ellipticities (b/a) of 10 selected stars in N242W bands are plotted with their distance from the field center. The adjacent histogram shows the distribution of measured ellipticity of the selected stars. The error bar plotted on the bottom left shows typical error in the estimated ellipticity.
Paper: The AstroSat UV Deep Field North: The Far- and Near-ultraviolet Photometric Catalog
Authors: Chayan Mondal, Kanak Saha, Souradeep Bhattacharya, Anshuman Borgohain, Shyam N. Tandon, Marc Rafelski, Rolf A. Jansen, Rogier A. Windhorst, Harry I. Teplitz, Brent M. Smith
Figure caption: A selected region in the GOODS-N field is shown as observed in different filters by GALEX (FUV, NUV), AstroSat/UVIT (F154W, N242W), and HST (F435W, F160W). The figure highlights the difference in angular resolution for three different telescopes. The size of the PSFs is indicated by blue circles in each panel. Both the HST PSF sizes are shown with 10× enhanced size.