adsabs/AstroCLIMB huggingface dataset:
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Mass distribution (left), radius distribution (center), and virial parameter distribution (right) of the clumps in the 27 GMCs, respectively. The blue and red line outlines represent the starless clumps and star-forming clumps in the GMC, respectively.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Correlation analysis between the DGMF of GMCs and the proportion of clumps capable of forming massive stars in the mass–radius relationship: starless clumps (blue) and star-forming clumps (red).
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Mass–radius relationship between clumps on the filaments and clumps off the filaments.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: DGMF of 27 GMCs. The red line represents the dense gas component ratio of GMCs calculated through mass, while the blue line represents the dense gas component ratio of GMCs calculated through pixel count.
Paper: Chasing the Neutrino Blazar Candidates
Authors: Jingtian Zhu, Haitao Cao, Hubing Xiao, Zhiyuan Pei, JunHui Fan, Denis Bastieri
Figure caption: The top panel shows the samples of 4FGL_DR3: 35 NBs, 3708 non-NBs, 625 nonblazars, and 2291 other sources. The bottom panel shows the 35 NBs and 625 nonblazars divided into four data sets: the training set consisting of 304–412 sources for pretraining, the validation set consisting of 98 sources for monitoring performance during training, the support set consisting of 18–126 sources for providing embedding templates, and the query set consisting of 132 sources for determining the K value in our two-way K-shot task.
Paper: Chasing the Neutrino Blazar Candidates
Authors: Jingtian Zhu, Haitao Cao, Hubing Xiao, Zhiyuan Pei, JunHui Fan, Denis Bastieri
Figure caption: The top panel shows the ANN (triplet network) pretraining process with triplet loss. Random triplets are selected from the training set, and the ANN with the smallest triplet loss on the validation set is chosen. The bottom panel demonstrates the use of the trained ANN to transform the support set and query set into the embedding space, where their similarity score is calculated. In the two-way K-shot process, the softmax function is taken as J(·) to calculate the similarities, as shown in Equation (6). While in the identification process, J(·) becomes cosine similarity for further analysis, as shown in Equation (7).
Paper: Chasing the Neutrino Blazar Candidates
Authors: Jingtian Zhu, Haitao Cao, Hubing Xiao, Zhiyuan Pei, JunHui Fan, Denis Bastieri
Figure caption: Probability of each blazar being an NBC. The x-axis represents all blazars, while the y-axis shows the probability of each blazar being an NB. Error bars marked in blue indicate the uncertainty in the probability estimates. The red dashed line represents a similarity score of 0.98, marking the threshold for selecting NBCs. The green dashed line indicates the starting point, with 199 sources to the right identified as NBCs.
Paper: Chasing the Neutrino Blazar Candidates
Authors: Jingtian Zhu, Haitao Cao, Hubing Xiao, Zhiyuan Pei, JunHui Fan, Denis Bastieri
Figure caption: The distribution histograms for the 35 NBs are red, blue for the 2244 non-NBs, and green for the 87 NBCs.
Paper: Chasing the Neutrino Blazar Candidates
Authors: Jingtian Zhu, Haitao Cao, Hubing Xiao, Zhiyuan Pei, JunHui Fan, Denis Bastieri
Figure caption: The F  β  scores for different K-shot configurations, with β ranging from 1 to 5, represented by blue, orange, green, red, and purple lines, respectively. The shaded areas around the lines indicate the standard deviation.
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Comparison of the spatial resolution of XMM-Newton (left) and Chandra (right); a 1′ scale bar is shown in both images. Left: the GL 412 binary star system with the locations of GL 412A (M1V) and GL 412B/WX Ma (M6.6V) shown by cyan circles. The circles have radii of 10″ and are separated by ∼30″ . A third, unidentified X-ray source (dashed yellow circle) is located ∼37″ from GL 412B. Right: the 40 Eri triple star system with the locations of 40 Eri A (K0V), 40 Eri B (DA white dwarf), and 40 Eri C (M4.5V) circled in white. The separation between the B and C components is ∼7″. X-ray sources are found coincident with 40 Eri A and C, while 40 Eri B is undetected.
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Left: photon arrival time CDF of Proxima Centauri (XMM-Newton observation ID 0801880501, black) compared to a constant count rate (dark red, dashed). The A 2 statistic and critical values are shown in the upper-left corner. Right: the light-curve data (black circles) compared to a constant count rate (dark red, dashed), with sections of the light curve color coded by VarFlag. Quiescent periods are shown in dark blue-violet (“Q”), flaring periods in pink “F”), and descending count rates in purple (“D”).
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Best-fit VEMs and temperatures for thermal plasma components from XSPEC modeling. VEMs and temperatures from APEC #1 are shown in circles, those from APEC #2 are shown in squares, and those from APEC # are shown in diamonds. Values measured for F and G stars are shown in yellow, K stars in orange, and M stars in red. M stars exhibit the largest variations in both VEM and temperature across all three APEC components.
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Best-fit spectra for all 38 XMM-Newton observations of ι Hor (black) with the average best-fit spectrum superimposed (red).
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Images of resolved and unresolved binary systems with XMM-Newton and Chandra. (a) XMM-Newton/PN image of υ And. The locations of the F8V star (A) and the M4.5V star (B) are shown by cyan circles (both with radii 10″). The stars are separated by ∼0.′9. (b) XMM-Newton image of GL 620.1A and the white dwarf WD 1620-391. No X-rays are detected at the location of WD 1620-391 in either observation. (c) The α Cen binary system as seen by the PN camera on XMM-Newton. The positions of the G2V star (A) and K1V star (B) are shown in blue circles (both with radii of 5″ and separated by ∼18″ ). (d) The ξ Boo binary system as seen by the MOS2 camera on XMM-Newton. The locations of the G8V star (A) and K4V star (B) are shown in cyan circles (both with radii of 5″). (e) The 70 Oph binary star system as seen by the PN camera on XMM-Newton. The positions of the K0V star (A) and the K5V star (B) are shown in blue circles (both with radii of 5″ and separated by ∼3.″7 ). (f) The GL 783 binary star system as seen by the PN camera on XMM-Newton. The positions of the K3V star (A) and the M4.5V star (B) are shown in cyan circles (both with radii of 5″ and separated by ∼2.″6 . (g) Chandra image of the GL 570 system. The primary GL 570A (K4V) is easily resolved from the binary red dwarf pair GL 570BC (M1.5V and M3V, respectively). Cyan circles have a radius of 10″. The brown dwarf GL 570D is not detected in X-rays. (h) The 61 Cyg binary system as seen by the PN camera on XMM-Newton. The positions of the K5V star (A) and K7V star (B) are shown in cyan circles (both with a radius of 10″ and separated by ∼12″). (i) Chandra image of Wolf 1055 and VB 10 (both circles have radii of 10″ and are separated by ∼1.′2). Some images have been smoothed for display purposes only; white contours indicate the intensity distribution of X-ray counts on the detector.
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: The L X/L bol ratio as a function of T eff. Stars in our sample with firm X-ray detections are shown in circles, while upper limits are shown for stars that were not X-ray detected (downward pointing triangles). Stars that are believed to be young (≲2 Gyr) are shown in red, older stars (≳2 Gyr) are shown in purple, and stars without age estimates or with ambiguous/discrepant age estimates are shown in dark blue. The MUSCLES/Mega-MUSCLES sample (A. Brown et al. 2023) is shown in gray. The yellow circles and shaded area indicate the quiescent and flaring L X/L bol ratios for the Sun (J. L. Linsky et al. 2020).
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Top: the fraction of time that a star is observed to be fainter than a specific luminosity. Bottom: the fraction of time that a star is observed to be below an L X/L bol value. Stars are color coded by spectral type, with earlier-type stars shown in yellow and later-type stars shown in dark red. The 25th, 50th, 75th, and 90th percentile luminosities and L X/L bol ratios are indicated by blue dashed lines (values for each star summarized in Table 7). The shaded gray region indicates typical ranges for the current Sun, and the blue shaded regions indicate approximate ranges for the early Sun (∼4 Gyr ago; see the text).
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Top: quiescent (solid lines) and flaring (dashed lines) continuum spectra of three representative stars from our sample (κ 1 Cet in yellow, GJ 570 A in orange, and Prox Cen in red). Bottom: the ratio of flaring spectrum to quiescent spectrum, showing a pronounced enhancement in X-ray emission at <10 Å during flaring periods for all three stars. The flaring spectrum of Prox Cen remains an order of magnitude brighter than the quiescent spectrum even at longer wavelengths.
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Top: the L X/L bol ratio as a function of T eff assuming L 25 (black), L 50 (blue), L 75 (green), and L 90 (dark yellow). The yellow circles and shaded area indicate the quiescent and flaring L X/L bol ratios for the Sun (J. L. Linsky et al. 2020). Bottom: the ratio of L 75/L 25 as a function of T eff, color coded by age (as in Figure 10: young stars are shown in red, old stars are shown in purple, and stars with ambiguous ages are shown in dark blue).
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Average continuum quiescent spectra for each target star (0.5–150 Å, corresponding to an energy range of ∼25–0.08 keV). Spectra have been corrected for minor foreground absorption. Stars are color coded by spectral type, with earlier-type stars shown in yellow and later-type stars shown in dark red.
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: The light curve of κ 1 Cet from XMM-Newton observation 0111410101. The MOS1 count rates were converted to luminosities (gray circles) using the best-fit spectral models from three subexposures (from 0–14 ks, 14–25 ks, and 25–39 ks). The Bayesian blocked light curve is superimposed in blue.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: MWL light curves from the 2018 April–2023 December observations. (a) XRT, (b) MAXI, (c) BAT, (d) LAT, (e) FACT, (f)–(k) UVOT UVW2–V bands. While the XRT, MAXI, FACT, and UVOT (next page) data are derived by using the 1 day integration, the BAT and LAT light curves are based on data binned every 1 week. In panels (b)–(c), the black and gray data points correspond to the detections of the source with 5σ and 3σ–4σ significances, respectively. In panel (d), the downward red triangle shows an upper limit to the 0.3–300 GeV flux when TS < 9 and/or N pred < 8. The vertical dashed line denotes a boundary between the different time intervals listed in Table 4.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Distribution of the MWL flux values: 1 day binned unabsorbed XRT-band flux in the entire 2018 April–2023 December period are presented in panel (a), while the subsamples from Intervals 1, 2, 5–6 and 2, 4, 7–8, as well as from those XRT observations showing the 0.3–10 keV IDVs (corresponding to each spectrum)—in panels (b)–(d); 1 day binned MAXI, FACT, UVOT-UVW1, and optical V-band (ground-based telescopes) fluxes—panels (e), (h), (i), and (j), respectively; 1 week binned BAT and LAT-band fluxes—panels (f)–(g). The red and green curves show the lognormal and Gaussian fits to the histograms, respectively.
Paper: Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Correlation between the MWL fluxes. (a) Unabsorbed 0.3–2 keV and 2–10 keV fluxes; (b)–(c) 0.3–10 keV flux vs. the 0.3–300 GeV (2 days of binned) and FACT-band (1 day binned) fluxes; (d)–(g) UVW2-band flux vs. the UVW1, 0.3–10 keV, V band, and 0.3–300 GeV fluxes; (h) V-band flux vs. 0.3–300 GeV flux. The black, red, blue, purple, green, orange, brown, and gray points correspond to the data from Intervals 1, 2, 3, 4, 5, 6, 7, and 8, respectively.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: Top left: Optical CMD using Gaia colors BP − RP vs. G magnitude of all the sources of the 12 globular clusters. The gray dots are the Gaia sources from H. Baumgardt & E. Vasiliev (2021), and the black circles, red triangles, and blue diamonds are the HB, BS, and post-HB stars observed in the CaF2 filter. Top right: The UV–optical CMD plots of CaF2, BaF2, Sapphire, and Silica filters are shown from left to right. We plot the absolute magnitude of the respective filters on the y-axis. The solid lines represent the zero-age HB (ZAHB) loci at [Fe/H]= −1.20 (cyan), −1.30 (orange), −1.55 (green), −1.70 (blue), −1.90 (magenta), and the red dashed line represents the TAHB line at [Fe/H] = −2.20. Bottom left: Optical CMD of all the open clusters observed in UVIT. The gray dots are the cluster members from T. Cantat-Gaudin et al. (2018). We have separated the sources observed in the NUVN2 filter into various evolutionary phases: BS (blue boxes), main-sequence (MS; orange dots), main-sequence turn-off (MSTO; cyan stars), RGB (red diamonds), subgiant (green crosses), spectroscopic binary (magenta upward triangles), blue supergiant (purple downward triangle), and subdwarf stars (brown hexagons). Bottom right: The UV−optical CMD plots of CaF2, Sapphire, NUVB13, and NUVN2 from left to right. We plot the absolute magnitude of the respective filters on the y-axis. The BaSTI isochrones are plotted at [Fe/H] = −1.25 (dotted line), +0.02 (dashed line), +0.03 (dashed dot line), +0.12 (solid line).
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: We crossmatch the noncrowded UVIT field sources in our catalog with SIMBAD. The difference in their aperture magnitude (aperture radius = 3 pixels) and Kron magnitude are shown in the left panel. The gray and green contours represent the confirmed stars and galaxies from the SIMBAD catalog. We calculate the m  μ  and m  σ  for (m Kron − m Aperture) in each magnitude bin of bin width = 0.5 mag. The red solid line shows the m  μ  line, and the black dashed line shows the m  μ  ± m  σ  lines. The sources between these lines are classified as probable point sources, while the rest are probable extended sources.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: Left: Magnitude difference between Kron elliptical magnitudes and the aperture magnitude (aperture radius = 3 pixels) for the sources observed in the BaF2 filter. The red boxes represent the confirmed stars from the SIMBAD catalog. We find that 90% of the stars have the ﹩{{m}}_{{\rm{Kron}}}-{{m}}_{{\rm{Aperture}}}\geqslant -1﹩ mag. The sources with the same magnitude difference are classified as point sources (blue solid circles) in gaseous nebulae, and the rest as extended clumps (black solid circles). Middle: the histogram plot of the number of point sources in different filters of gaseous nebulae fields. Right: the histogram plot of the number of clumps in different filters of gaseous nebulae fields.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: Image of a few astrophysical objects observed by UVIT in FUV and NUV filters. Left: UVIT observation of globular cluster NGC 288 (G05_009T02). The red, blue, and black circles represent the r  c , r  h , and R (radius within which the sources are unresolved by the SE), respectively. Middle: point sources and clumps in gaseous nebula NGC 6995 (G06_060T01). Right: clumps in the nearby galaxy NGC 1365 (A02_060T01).
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: The area covered by M31 FoVs observed by UVIT in various UVIT filters and the black solid circles show the FoV of the image. The red dots are the UV sources in UVIT DR1 overlapped with the UV source catalog published by D. A. Leahy et al. (2020; represented by gray dots). The blue dots are the sources in UVIT DR1, which are observed by other PIs. In the right panel, we show the magnitude difference between UVIT DR1 and UV source catalog published in D. A. Leahy et al. (2020) for a single M31 field (A04_022T07). The magnitude difference increases in the crowded regions.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: The top panel shows an Aitoff projection of the central celestial coordinates for the 291 fields observed in the year 2016–2017 by UVIT. In the bottom panel, Venn diagrams show the distribution of all UVIT observations in different filters. The bottom left panel is for FUV observations, and the bottom right panel is for NUV observations.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: We fit the Gaussian functions on the histograms of the mean μ (left panel) and mean σ (right panel) calculated for each 21 × 21 pixels box in an image. The vertical lines display mean μ and mean σ values for an FUV observation determined from the Gaussian fits.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: Example of various artifacts observed in UVIT images. Left: artifacts caused due to large satellite trails. Middle: artifacts caused due to fast moving satellites. Right: artifacts caused due to a bright galaxy.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: Magnitude histograms in various FUV (left panel) and NUV (right panel) filters of UVIT. The dashed lines represent the peak magnitudes of the respective filters, which determines the magnitudes at which most sources are detected. The filter names, along with the number of sources detected, are mentioned in the legend.
Paper: A Comprehensive Catalog of UVIT Observations. I. Catalog Description and First Release of Source Catalog (UVIT DR1)
Authors: Sonika Piridi, Ranjan Kumar, Divya Pandey, Ananta C. Pradhan
Figure caption: FUV−NUV histogram for clumps commonly detected in BaF2 and Silica15 filters. The gray dashed line at color FUV−NUV = 0.9 mag segregates young and old stellar population-dominated galaxies (A. Gil de Paz et al. 2007).