adsabs/AstroCLIMB huggingface dataset:
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Positions of limbs observable during ingress and egress on the planet, as expected from the orbital parameters of WASP-39 b. Panel (a) is similar to panel (b) of Figure 1, but the xi-axis and yi-axis are colored blue, and the xe-axis and ye-axis are colored orange. The blue and orange points indicate where the limbs intersect the xi-axis or xe-axis. The open points represent those on the dayside of the northern hemisphere, while the filled points represent those on the nightside of the southern hemisphere. The limb observable during ingress is colored blue, and the limb observable during egress is colored orange. Panels (b), (c), and (d) show the positions of the xi-axis, yi-axis (blue), xe-axis, and ye-axis (orange) and the limbs observable during ingress (blue belt) and egress (orange belt) on the planet. The finite width of each belt reflects the shift caused by the planet’s rotation during ingress or egress. The white and gray hemispheres represent the dayside and nightside of the planet, respectively. Panel (c) shows the view from the nightside, and panel (d) shows the view from the north. The limbs observable during ingress and egress are shifted slightly away from the terminator. The yi-axis and ye-axis intersect the terminator.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Light conditions of the atmosphere transmitted by the host star’s light during ingress (left) and egress (right), as expected from the orbital parameters of WASP-39 b. The yi-axis (for ingress) and ye-axis (for egress) are normal to the plane of the paper and directed out of the page. The white and gray semicircles represent the planet’s dayside and nightside, respectively. The yellow and purple regions represent the atmosphere of the dayside and nightside, respectively. The blue and orange points indicate where the limbs observed during ingress or egress intersect the xi-axis or xe-axis. Open points represent positions in the positive xi- or negative xe-directions, while filled points represent those in the negative xi- or positive xe-directions. Dashed arrows show the direction toward the center of the host star and the observer, which are not aligned. Therefore, the light conditions of the atmosphere at the positive xi limb vs. the negative xi limb or at the positive xe limb vs. the negative xe limb are different. The atmosphere between the dashed lines on each limb contributes to the transmission spectrum.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Changes in timing and duration of ingress caused by atmospheric asymmetries. The colored solid lines and gray dashed lines in the graphs on the right correspond to the light curves of the planet’s shadow disks with the same color in the schematics on the left, respectively. Thin gray lines in the schematics on the left show the lines of constant ﹩{t}_{i}^{{\prime} }(\sim {t}_{{\rm{i}}})﹩ or τi. (a) Asymmetry in the direction of orbital motion preserves the duration of ingress τi. The colored dotted lines in the schematics on the left show the lines of constant ﹩{t}_{i}^{{\prime} }﹩ for each planet’s shadow disk. (b) Asymmetry along the host star’s edge preserves the timing of ingress ﹩{t}_{i}^{{\rm{{\prime} }}}﹩. The colored dotted lines in the schematics on the left show the lines of constant τi for each planet’s shadow disk.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of k = Rp/Rs and the contact times tI, tII, tIII, and tIV for three symmetric planets with ﹩(e\cos \omega ,\,e\sin \omega )=(0,\,0)﹩, (0.1, 0), and (0, 0.1), based on the MCMC analysis of simulated data. The circular orbit model was used to derive these values in the MCMC analysis. The dots represent the median values from the MCMC sampling, while the error bars indicate the 68% credible intervals. Results are shown for both noiseless data and data with added Gaussian noise (mean = 0, standard deviation = 250 ppm), along with the true values.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of ΔcX and ΔcY during ingress and egress for three symmetric planets with ﹩(e\cos \omega ,\,e\sin \omega )=(0,\,0)﹩, (0.1, 0), and (0, 0.1), based on the MCMC analysis of simulated data. The values converted using both estimated and true orbital parameters are shown. The circular orbit model was used to derive these values in the MCMC analysis. The dots represent the median values from the MCMC sampling, and the error bars indicate the 68% credible intervals. Results are shown only for noiseless data, along with the true values.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩, and ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩ for three symmetric planets with ﹩(e\cos \omega ,\,e\sin \omega )=(0,\,0)﹩, (0.1, 0), and (0, 0.1), based on the MCMC analysis of simulated data. The values were converted using the estimated orbital parameters. The circular orbit model was used in the MCMC analysis to derive these values. The dots represent the median values from the MCMC sampling, while the error bars indicate the 68% credible intervals. Results are shown for both noiseless data and data with added Gaussian noise (mean = 0, standard deviation = 250 ppm), along with the true values.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Simulated noiseless light curves of symmetric planets with elliptical orbits (black dots) and fitted light curves using the circular orbit model (orange lines). The bottom panels show the residuals. (Top) Case of ﹩(e\cos \omega ,\,e\sin \omega )=(0.1,\,0)﹩. (Bottom) Case of ﹩(e\cos \omega ,\,e\sin \omega )=(0,\,0.1)﹩.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Moment maps and spectra for a set of detections with extreme asymmetries, labeled A–E in Figure 9 to illustrate different drivers of asymmetry. The cyan circles in the lower left of the moment 0 map panels show the size of the beam. The magenta x symbols and vertical lines in the maps and spectral plots show the SOFIA-2 center. This center is used for the calculation of the asymmetries listed in the moment 0 plot (3D) and spectra (1D).
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Histograms of the properties of WALLABY detections. The dashed black lines show the full set of detections where kinematic modeling was attempted. The blue shaded regions show those detections where the kinematic modeling was successful and they have measured asymmetries, while the red shaded region shows those where the kinematic modeling failed but they still have measured asymmetries. In the top three rows, the ratio of the red plus blue histograms (the solid black line) to the dashed histogram is equal to the fraction of galaxies for which asymmetries were measured.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Comparison of the 1D and 3D asymmetries of WALLABY detections with ﹩{\mathrm{log}}_{10}({M}_{\,\rm{H}\,\,\rm{I}}/{M}_{\odot })\geqslant 9﹩. The size of the points correlates to their size on the sky, and the colorbar identifies their S/N. The stars show galaxies where kinematic modeling is successful, while the circles show those without kinematic models. Maps and spectra for the detections labeled A, B, C, D, and E are shown in Figure 10.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Map of the asymmetry distributions for the WALLABY sample and the WALLABY-like SIMBA mocks. The cyan contours draw the SIMBA distribution for the count-wise 68th, 95th, and 99th percentiles. The orange dots are the individual WALLABY measures. The underlying map shows the mean p-value for binomial tests averaged across different binnings of the A1D–A3D plane.
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: Comparison of the radial velocities, observed (Vr) and expected (﹩{V}_{{\rm{\exp }}}﹩), for M31 and MW objects, represented by red plus signs and blue circles, respectively. The velocity difference (Vr − ﹩{V}_{{\rm{\exp }}}﹩) is plotted against ﹩{V}_{{\rm{\exp }}}﹩. The median values of velocity difference for M31 and MW objects are shown by the red and blue solid curves, respectively, with the red and blue dashed curves representing the 3σ scattering of data points. The red solid straight line indicates a constant ﹩{V}_{r}-{V}_{\exp }﹩ = 271.9 km s−1 for M31 objects, and the blue solid straight line shows Vr =  −149.5 km s−1 for the MW objects. The black lines indicate the criteria (after correction) given by M. R. Drout et al. (2009).
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: Spatial distributions of classified emission-line nebulae observed with LAMOST, overlaid on the mosaicked images of M31 and M33 as retrieved from the Digitized Sky Survey. Top panels: spatial distributions of PNe (left panel, small circles) and H II regions (right panel, small squares) in M31. Bottom panels: same as the top panels, but for M33. Color-coding of the data symbols represents weighted radial velocity after subtracting the systemic velocity (Vr) of the host galaxy. A systemic velocity of  −179 km s−1 for M33 was adopted.
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: Spatial distribution of supergiants and candidates in M31 as identified from the LAMOST database, overlaid on the Herschel SPIRE 250 μm image (J. Fritz et al. 2012). Objects are color-coded according to the probability of M31 membership (PM31, values scaled from 0 to 1); a few objects that lack accurate radial velocity information are shown in white.
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: BPT diagram of the emission-line nebulae in our catalog. The nebulae in M31 are shown as red squares, and those in M33 are shown as blue triangles. The black solid line represents our criterion for distinguishing PNe from H II regions. The gray dashed line reflects the demarcation given by A. Y. Kniazev et al. (2008).
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: Top: distribution of the probability of M31 membership (PM31, values scaled from 0 to 1) of our newly identified supergiant candidates (in black), along with known supergiants and candidates (in gray). Bottom: distribution of (﹩{V}_{r}-{V}_{\exp }﹩) for the known and newly identified supergiants and candidates, with the same color-coding as above.
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: LAMOST spectra of two dual-velocity objects. The two velocity components are color-coded for clarity: blue indicates the blueshifted component, while red signifies the redshifted component. Object J004301.10+410642.8 (top two panels), a PN candidate from M06, shows a velocity disparity of  ∼280 km s−1. Object J004192.85+405048.1 (bottom two panels), identified as an H II region in M31, displays a velocity difference of 528 km s−1.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Two-color images of a few sources in our catalog with interesting morphological features. In all images, the NUV wave band image (smoothed using a Gaussian filter with FWHM of 1.2″) is shown in red and the FUV band image (smoothed using a Gaussian filter with FWHM of 2.0″) is shown in blue.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Comparison of observed FUV-Gaia and NUV–Gaia colors with that predicted for type 1 AGNs with a range of accretion disk temperatures kTin = 2 − 14 eV and redshifts z = 0.0 − 2.9. The similarity of the location of the observed colors and the simulated colors strongly suggests that the UVIT sources are type 1 AGNs. The numbers annotated to the observed data points show the ID for that source in our catalog.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Upper panel: Theoretical spectrum of an accretion disk derived from the XSPEC model diskbb with an inner-disk temperature of 10 eV. Fλ is the flux density for an arbitrary normalization of the diskbb model. Lower panel: The effective area as a function of wavelength for the FUV/F154W, NUV/N245M, and Gaia G-band filter. The effective area for the Gaia G band is the product of the filter transmissivity and the telescope pupil area (see Section 4.2).
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Left panel image shows the two FUV sources that have both been identified with a single NUV source shown in the right panel image. The green ellipse shows the source region, and the number next to it is the ID of that source in that particular (FUV or NUV) catalog. In the FUV field image we can see two sources with overlapping light profile but with distinguished core regions indicating the presence of two sources, although in the NUV image these two sources cannot be identified separately.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: The growth curves (blue) for the NUV (left panel) and FUV (right panel) bands, showing the fractional enclosed flux as a function of radius in pixels. Each pixel measures 0.416″.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: The histogram of the CLASS_STAR value given by SExtractor for all the Gaia stars present in our catalog. The Gaia sources for which the measured value of any of the two components of proper motion is significant above the 3σ level are considered stars.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: NUV light curves of 25 point sources that are variable in NUV above a 2.5σ significance level but are not variable in the FUV band. The Julian date of our observation is shown on the x-axis, and the NUV count rates for the sources are plotted along the y-axis. In the header of each plot the source ID is mentioned along with their probable classification in the bracket.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Histogram of UV color (mFUV − mNUV) for all 456 sources in our catalog that are detected in both the NUV and FUV bands above the SNR of 5. A total of 17 sources are found with negative color values, that is, they are brighter in the FUV than in the NUV band.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Light curves of three point sources that are variable above the 2.5σ significance level in both the NUV and the FUV bands. Upper panel: NUV light curves for these three sources. Lower panel: FUV light curve of the corresponding source. In the header of each panel the source ID is mentioned along with their probable classification in the bracket.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: In the left-hand diagram, we plot the log([N II]/Hα) values for spaxels labeled as HEW. Similarly, in the right-hand panel, we plot the equivalent width values for spaxels labeled as HEW in units of angstrom.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: WHAN plot divided by structures. We show the ensemble of points color coded to each structure studied in detail in Section 4.2. For each structure, the mean value with a 1σ error is superimposed on the data points.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: The left panel is a diagram of the shock region in NGC 1275. The background image is the Chandra soft X-ray emission between 0.5 and 2.0 keV described in Section 2.2; the contours highlight the Hα emission. We highlight the location of the shock front (blue) as detected in A. C. Fabian & J. S. Sanders (2006). In the right-hand panel, we show the WHAN plot for the bar in the shock region (orange) and the small northern filament (green) that has not yet gone through the shock.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: The left panel is a diagram of the central region of the filamentary nebula in NGC 1275. The background image is the Chandra soft X-ray emission, while the white contours highlight the Hα emission. We partition the central region into the high dispersion region as initially discovered in B. Vigneron et al. (2024) and the remaining pixels. We show the WHAN diagram for the high dispersion component (blue) and the remaining spaxels in the central region (orange). The right-hand panel shows the WHAN plot color coded by distance to the AGN.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: Diagram and WHAN plot of the horseshoe region of the NGC 1275 filamentary nebula. The background image is the Chandra soft X-ray emission, while the white contours highlight the Hα emission. The horseshoe is segmented into four color-coded sections, capturing the different morphological regions of the area. The colors on the diagram correspond to those in the WHAN plot.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: The left-hand plot is a diagram of the larger northern filament. The background image shows the soft X-ray emission captured by Chandra, with white contours following the Hα emission. The WHAN plot on the right is color coded by the distance to the bottom of the filament.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: WHAN diagram and color-coded map for all pixels in the nebula surrounding NGC 1275 with an SNR over 3 and flux over 1e−17 erg s−1 cm−2 Å−1. The pixels are divided into three categories: star forming (orange), HEW (teal), and LEW (purple). Measurements below the dotted line are considered uncertain (R. Cid Fernandes et al. 2011).