adsabs/AstroCLIMB huggingface dataset:
Paper: HST Proper Motions of Andromeda V and Andromeda VI
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Max Martone, Alexander Petroski
Figure caption: The M31-centric distance and total velocity of And V and VI using the HST+Sats M31 proper motion (blue square) and its weighted average with EDR3 (black diamond). Escape velocity curves of the two M31 mass models adopted in this paper are shown as solid and dashed lines, while a Milky Way-like potential is displayed for reference (gray dotted line). Results for NGC147, NGC185, and And III, three other M31 satellites with published proper motions, are also shown in pink, yellow, and teal, respectively.
Paper: HST Proper Motions of Andromeda V and Andromeda VI
Authors: Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke Jamie Kanehisa, Max Martone, Alexander Petroski
Figure caption: Same as in Figure 6, only for And VI.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: Our measurements of the rest-UV luminosity functions based on JADES data. We show F115W dropout luminosity function (zmedian = 9.8, N = 309) in the top-left panel, the F150W dropouts (zmedian = 12.8, N = 63) in the top-right panel, the z ≥ 14 subset of the F150W dropouts (zmedian ∼ 14.3) in the bottom-left panel, and the upper limits based on the absence of F200W dropouts (z ∼ 16–22.5) in the bottom-right panel. Due to the method we use to calculate the z ≥ 14 F150W dropout luminosity function, described in Section 5.2, the number of objects is not well defined. We show our binned measurements as green hexagons, the Schechter fits as solid green lines, and the DPL fits as dashed green lines. For comparison, we show the luminosity functions at the central redshifts of the dropout samples predicted by the fits for the redshift evolution of the Schechter (R. J. Bouwens et al. 2021) and DPL (R. A. A. Bowler et al. 2020) parameters, which were determined from HST and ground-based data. We also show measurements from R. A. A. Bowler et al. (2020), R. J. Bouwens et al. (2021), G. C. K. Leung et al. (2023), P. G. Pérez-González et al. (2023), Y. Harikane et al. (2023, 2024a), N. J. Adams et al. (2024), C. J. Willott et al. (2024), S. L. Finkelstein et al. (2024), C. T. Donnan et al. (2024), B. Robertson et al. (2024), V. Kokorev et al. (2024), P. G. Pérez-González et al. (2025), M. Castellano et al. (2025), and A. Weibel et al. (2025) at the redshifts closest to the central redshift of the F115W and F150W dropout samples (typically z = 9 or 10 for the F115W dropouts, z = 12 or 12.5 for the F150W dropouts, z = 14 or 14.5 for the z ≥ 14 F150W dropouts, and z = 16, 17 and 17.5 for the F200W dropout upper limit). In general, we find broad agreement with existing measurements of the luminosity function with smaller uncertainties.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: A comparison of our measured F115W dropout, F150W dropout, and z ≥ 14 F150W dropout luminosity functions with various theoretical models as colored regions: with hatches for models from before JWST (P. Behroozi et al. 2020; R. Kannan et al. 2022; J. Rosdahl et al. 2022; S. M. Wilkins et al. 2023), and solid colors for models published after JWST (A. Dekel et al. 2023; G. Sun et al. 2023; V. Gelli et al. 2024; Z. Li et al. 2024; L. Y. A. Yung et al. 2024; R. Feldmann et al. 2025). We show the binned data as black hexagons and the Schechter fits as black lines. We do not fit a Schechter function to the z ≥ 14 luminosity function but show the F150W dropout luminosity function as a dashed line for comparison. The upper and lower bounds of the model regions correspond to the predicted luminosity functions for the redshifts that bracket the central redshift of our observed luminosity function (e.g., we often show z = 9 and z = 10 for the F115W dropouts). Our observed luminosity functions are consistent with some models at z ∼ 10. However, at z ≳ 12, the observations lie increasingly above model predictions at all luminosities we have examined in this work.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: The distribution of redshifts (spectroscopic redshifts if available, otherwise photometric redshifts from BEAGLE) and absolute UV magnitudes for our three dropout samples. We show the F115W dropouts as blue diamonds and the F150W dropouts as dark-green circles with corresponding colors for the histograms. Objects with spectroscopic redshifts are outlined in black. We also show the 2D detection and selection completeness measured as described in Section 5.1 as a function of F277W apparent magnitude and redshift in the background. Darker gray indicates a higher completeness. The F115W dropouts span absolute UV magnitudes of −16.8 ≤ MUV ≤  −21.7 (median MUV = −18.5) and redshifts of z = 8.4–12.1 (median z = 9.8), consistent with expectations from our selection function. The F150W dropouts have absolute UV magnitudes of −17.4 ≤ MUV ≤  −20.8 (median MUV = −18.5) and redshifts of z = 11.1–15.3. We note that we attribute the apparent weighting of the observed samples toward the lower redshifts and fainter luminosities of the selection functions to the larger numbers of these objects (i.e., at fixed completeness, we will identify more faint, lower-redshift candidates compared to brighter, higher-redshift systems). We note that GN-z11 (P. A. Oesch et al. 2016; A. J. Bunker et al. 2023) is the brightest object in the F115W dropout sample, and JADES-GS-z14-0 (S. Carniani et al. 2024b) is the brightest object in the F150W dropout sample.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: The cosmic UV luminosity density integrated to MUV = −17 (left y-axis) and converted to ρSFR (right y-axis) with the factor ﹩{ \mathcal K }=1.15\times 1{0}^{-28}﹩ (M⊙ yr−1) / (erg s−1 Hz−1) (P. Madau & M. Dickinson 2014). For the F115W and F150W dropouts, we show the results of integrating the Schechter function fits. For the F200W dropout upper limit, we integrate the binned upper limits of the luminosity function between MUV = −21 and MUV = −17. For comparison, we show observational constraints based on HST and ground-based data (D. J. McLeod et al. 2016; P. A. Oesch et al. 2018; R. J. Bouwens et al. 2021) and JWST data (P. G. Pérez-González et al. 2023; N. J. Adams et al. 2024; C. T. Donnan et al. 2024; S. L. Finkelstein et al. 2024; Y. Harikane et al. 2024; B. Robertson et al. 2024; C. J. Willott et al. 2024). We also show theoretical predictions from a variety of models (P. Behroozi et al. 2020; G. Sun et al. 2023; S. M. Wilkins et al. 2023; A. Ferrara 2024; V. Gelli et al. 2024; L. Y. A. Yung et al. 2024; R. Feldmann et al. 2025). Consistent with other JWST measurements, we observe an excess in the cosmic UV luminosity density that is in increasingly strong tension with models at z ∼ 10.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: Postage stamps and CIRC1 SEDs of a subset of the F115W dropout sample ordered by decreasing UV luminosity from top to bottom and left to right. The postage stamps are 1″ on a side, and we show a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 scale bar on the S/N image for each object. For the SEDs, we show the observed photometry as the colored points (blue diamonds for NIRCam and purple squares for Advanced Camera for Surveys, ACS), the model photometry as the open black diamonds, and the median model spectra with errors as the black lines and gray shaded regions. When the observed photometry has S/N < 1, we show 2σ upper limits as open symbols. These objects span nearly five magnitudes in UV luminosity, are often observed with extremely red colors spanning the Lyα break (>2 mag), and generally have blue UV continuum slopes. The SEDs and postage stamps for all of our dropout candidates are available at https://github.com/lwhitler/jades_highz_uvlf.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: The distributions of observed F277W apparent magnitudes and rest-UV slopes, β, of our dropout samples. To measure UV slopes, we fit a power law of the form fλ ∝ λβ to three wide filters expected to probe the rest-frame UV; see Section 4 for details. We show the F115W dropout sample in blue with a solid outline and the F150W dropout sample in dark green with a dashed outline. The median values for the F115W and F150W dropout samples are shown as vertical lines. Our samples are relatively faint, with median F277W apparent magnitudes of mF277W = 29.2 and mF277W = 29.4 for the F115W and F150W dropouts, respectively. Consistent with expectations for high-redshift galaxies (e.g., F. Cullen et al. 2023; D. Austin et al. 2024; M. W. Topping et al. 2024), we also find generally blue UV continuum slopes with median β = −2.2 for the F115W dropouts and β = −2.1 for the F150W dropouts.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: The redshift evolution of the number densities of bright (MUV = −20.5, top) and faint (MUV = −18, bottom) galaxies. We show our measurements from the binned luminosity functions as dark-green hexagons (we note that the bright end of the z ≥ 14 F150W dropout luminosity function, with a median redshift of z ∼ 14.3, is dominated by JADES-GS-z14-0 and may not be broadly representative of the full galaxy population). We also show the measurement from the JADES Origins Field (B. Robertson et al. 2024) as a light-green hexagon, a compilation of measurements from the literature as yellow points (symbols as in Figure 6), and a comparison to the same models as in Figure 9. Consistent with many other observations of the high-redshift UV luminosity function from JWST, we find an excess of bright galaxies over all models at z ≳ 12. We also find a similar, though smaller, excess over most models at the faint end of the luminosity function.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: All of the UV luminosity functions we have measured in this work. We show the binned values for each of the dropout samples and the Schechter function fits for the F115W and F150W dropout samples. We show the F115W dropout luminosity function using blue diamonds and a solid line, the F150W dropouts as dark-green circles and dashed line, and the F200W dropout upper limits as the open, light-green squares. We also show the binned z ≥ 14 luminosity function, calculated as a subset of the F150W dropouts, as purple stars. We find mild evolution between the F115W and F150W dropout luminosity functions, stronger at the faint end than at the bright end, and little to no evolution between the full F150W dropout luminosity function and subset restricted to z ≥ 14.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: The same as Figure 3 for a subset of the F150W dropouts. The NIRCam photometry is shown as green circles, and the ACS photometry is shown as purple squares. The F150W dropouts span a range of 3.5 mag in UV luminosity and generally have blue UV continuum slopes.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: The timeline of reionization implied by the redshift evolution of the UV luminosity function. We show the results of all three luminosity function evolutionary fits (HST only as the dotted purple line, HST+JWST as the dashed blue line, and HST+JADES as the solid green line) for our fiducial assumptions of fesc = 0.1 and the ξion–MUV relation found by R. Endsley et al. (2024). To show the impact of the escape fraction and ionizing photon production efficiency, we also show the reionization timeline assuming the HST+JADES UV luminosity function evolution for fesc = 0.2 (thin, solid, light-green line) and constant ξion = 1025.8 Hz erg−1 (thin, dotted–dashed, light-green line). For comparison, we show observational constraints on the neutral fraction from galaxies (M. Ouchi et al. 2010, 2018; A. Konno et al. 2014; A. K. Inoue et al. 2018; C. A. Mason et al. 2018, 2019; A. Hoag et al. 2019; I. Jung et al. 2020; L. R. Whitler et al. 2020; H. Goto et al. 2021; A. M. Morales et al. 2021; P. Bolan et al. 2022; Y. Ning et al. 2022; S. Bruton et al. 2023; T. Morishita et al. 2023; T. Y.-Y. Hsiao et al. 2023; M. Nakane et al. 2024; H. Umeda et al. 2024; M. Tang et al. 2024) and quasars (X. Fan et al. 2006; I. D. McGreer et al. 2015; B. Greig et al. 2017; B. Greig et al. 2019, 2024; E. Bañados et al. 2018; F. B. Davies et al. 2018; F. Wang et al. 2020; J. Yang et al. 2020a, 2020b; Y. Zhu et al. 2022, 2024; X. Jin et al. 2023; D. Ďurovčíkova et al. 2024). When assuming an escape fraction of fesc = 0.2 or constant ξion = 1025.8 Hz erg−1, the large faint galaxy population produces more ionizing photons than is necessary to drive reionization, ending reionization earlier than is allowed by observational constraints (e.g., H. Atek et al. 2024; J. B. Muñoz et al. 2024). In contrast, reionization ends around z ∼ 5.3 for all models with our fiducial assumptions, approximately consistent with precise constraints on the end of reionization from quasars. However, though the end of reionization is largely insensitive to the UV luminosity function evolution, the HST+JADES fit starts reionization slightly earlier, leading to a neutral fraction of ﹩{\overline{x}}_{{\rm\small{HI}}}\sim 0.9\,\unicode{x02013}\,0.95﹩ at z = 10.
Paper: The z ≳ 9 Galaxy UV Luminosity Function from the JWST Advanced Deep Extragalactic Survey: Insights into Early Galaxy Evolution and Reionization
Authors: Lily Whitler, Daniel P. Stark, Michael W. Topping, Brant Robertson, Marcia Rieke, Kevin N. Hainline, Ryan Endsley, Zuyi Chen, William M. Baker, Rachana Bhatawdekar, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Eiichi Egami, Daniel J. Eisenstein, Jakob M. Helton, Zhiyuan Ji, Benjamin D. Johnson, Pablo G. Pérez-González, Pierluigi Rinaldi, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok
Figure caption: The redshift evolution of the Schechter parameters and the cosmic UV luminosity density. From left to right, we show the normalization, the characteristic luminosity, the faint-end slope, and the cosmic UV luminosity density. On the right y-axis of the rightmost panel, we also show the ionizing emissivity, ﹩{\dot{n}}_{\,\rm{ion}\,}﹩, that corresponds to the cosmic UV luminosity assuming a constant ionizing photon production efficiency of ξion = 1025.2 Hz erg−1 and escape fraction of fesc, which were shown to be sufficient to reionize the Universe given luminosity function constraints from HST (B. E. Robertson et al. 2013). We show three different evolutionary fits: HST only (R. J. Bouwens et al. 2021; dotted purple line and dark blue circles), HST and a compilation of JWST data including this work (dashed blue line, yellow symbols), and HST and JADES only (solid green line, green hexagons). The two fits that include JWST data have higher normalizations than the HST-only fit at z > 10 but slightly shallower faint-end slopes. However, the HST and JADES fit predicts steeper faint-end slopes than when including other JWST data. Together, the higher normalization and steep faint-end slope suggests the presence of a large population of faint galaxies producing copious amounts of nonionizing UV photons at early times (as seen in the cosmic UV luminosity density), which may play a significant role in reionization if they also produce ionizing UV radiation that can escape into the IGM.
Paper: Discovery of Giant Bubbles in the Hot Gaseous Halo of the Massive Disk Galaxy NGC 6286
Authors: Lin He, Zhiyuan Li, Zongnan Li, Rubén García-Benito, Yuanqi Liu, Meicun Hou
Figure caption: (a) DESI g-band image of the interacting system Arp 293 (NGC 6286/6285), overlaid with the VLA 3 GHz intensity contours at 5, 10, 20, and 50 times the rms level (0.04 mJy beam−1). The blue polygon outlines the CALIFA footprint. A prominent stellar feature located at in the southeast halo of NGC 6286 is reminiscent of a polar ring created by tidal interaction. The cyan cross marks the position of the radio core, which is significantly offset from the optical center (the magenta plus). (b) A tricolor composite image of Spitzer/IRAC 8 μm (red), DESI g-band (green), and Chandra 0.5–2 keV (blue), with the Hα line emission in white contours, at intensity levels of ﹩(1,2.25,6.75,20.25)\times 1{0}^{-18}\,{\rm{erg}}\,{{\rm{s}}}^{-1}\,{{\rm{cm}}}^{-2}\,{{\rm{arcsec}}}^{-2}﹩. The optical and infrared images suggest a strongly perturbed disk, likely due to tidal interaction. (c) Chandra 0.5–2 keV flux map zoomed-in to NGC 6286, with point sources subtracted. A Gaussian smoothing with kernel radius of 5 pixels is applied. The green ellipse has PA = 35°, ﹩a=0\mathop{.}\limits^{^{\prime} }65﹩, and ﹩b=0\mathop{.}\limits^{^{\prime} }16﹩, where PA, a, and b are the position angle, semimajor axis, and semiminor axis, respectively, adopted from the NASA/IPAC Extragalactic Database (NED) based on the Two Micron All Sky Survey Ks-band isophote of 20.0 mag ﹩{{\rm{arcsec}}}^{-2}﹩. The two magenta boxes outline the spectral extraction region for the X-ray bubbles. The cross and contours have the same meaning as panel (a). (d) Hα velocity map (relative to the systemic velocity) derived from the CALIFA datacube, with the same field of view as panel (c). Only pixels with an S/N larger than 5 are displayed. The color bar has units of km s−1. The cross marks the position of the radio core, and the contours have the same meaning as panel (b).
Paper: Discovery of Giant Bubbles in the Hot Gaseous Halo of the Massive Disk Galaxy NGC 6286
Authors: Lin He, Zhiyuan Li, Zongnan Li, Rubén García-Benito, Yuanqi Liu, Meicun Hou
Figure caption: Hα (left) and X-ray (middle) intensity maps zoomed to the bubble-like structures. The white rectangles parallel to the major axis have a size of 36″ × 14″, outlining the regions from which we extract the profiles. The gray solid (dashed) line indicates the major (minor) axis adopted from NED. Right: Hα (magenta) and X-ray (blue) surface brightness profiles of the bubble emission. The northern profile is defined to have a negative value to show the mirror symmetry. Four peaks corresponding to the bubble boundaries are unambiguous for the Hα emission, while their X-ray counterparts are less clear, especially in the north bubble.