adsabs/AstroCLIMB huggingface dataset:
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: PSD plots of the fluctuating velocity field over the same 30 minute Alfvénic slow solar wind used in Figure 7, showing (top-row panels): the fluctuating velocity field of the forward (solid curve) and backward (dashed curve) Alfvén modes (blue), fast (green), and slow (orange) magnetosonic modes as a function of frequency (f). Middle-row panels: the total velocity fluctuations of the forward and backward Alfvén spectra, fast, and slow magnetosonic modes as a function of parallel wavenumber (k∥) (left); the perpendicular velocity field fluctuations of the forward and backward Alfvén, fast, and slow magnetosonic modes as a function of parallel wavenumber (k∥) (center); the parallel velocity field fluctuations of the forward and backward fast, and slow magnetosonic modes as a function of parallel wavenumber (k∥) (right). Bottom-row panels: the total velocity fluctuations of the forward and backward Alfvén spectra, fast, and slow magnetosonic modes as a function of perpendicular wavenumber (k⊥) (left); the perpendicular velocity field fluctuations of the forward and backward Alfvén, fast, and slow magnetosonic modes as a function of perpendicular wavenumber (k⊥) (center); the parallel velocity field fluctuations of the forward and backward fast, and slow magnetosonic modes as a function of perpendicular wavenumber (k⊥) (right).
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: PSD plots of the fluctuating magnetic field over the same 30 minute Alfvénic slow solar wind used in Figure 7, showing (top-row panels): the fluctuating magnetic field of the forward (solid curve) and backward (dashed curve) Alfvén (blue) modes, fast (green), and slow (orange) magnetosonic modes as a function of frequency (f). Middle-row panels: the total magnetic fluctuations of the forward and backward Alfvén, fast, and slow magnetosonic modes as a function of parallel wavenumber (k∥) (left); the perpendicular magnetic field fluctuations of the forward and backward Alfvén, fast, and slow magnetosonic modes as a function of parallel wavenumber (k∥) (center); the parallel magnetic field fluctuations of the forward and backward fast, and slow magnetosonic modes as a function of parallel wavenumber (k∥) (right). Bottom-row panels: the total magnetic fluctuations of the forward and backward Alfvén spectra, fast, and slow magnetosonic modes and magnetic island modes as a function of perpendicular wavenumber (k⊥) (left); the perpendicular magnetic field fluctuations of the forward and backward Alfvén, fast, and slow magnetosonic modes as a magnetic of perpendicular wavenumber (k⊥) (center); the parallel magnetic field fluctuations of the forward and backward fast, and slow magnetosonic modes as a function of perpendicular wavenumber (k⊥) (right).
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis of the normalized magnetic field fluctuations over the eight 30 minute subintervals within fast interval. Top-left panel: parallel (z) magnetic field fluctuations for forward (black curve) and backward (orange curve; ±) fast MS modes ﹩\delta {B}_{z}^{{f}^{\pm }}/{B}_{0}﹩. Middle-left two panels: forward and backward transverse magnetic field fluctuations ﹩\delta {B}_{x,y}^{{f}^{\pm }}﹩ for fast MS modes. Bottom-left panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {B}_{x}^{{A}^{\pm }}﹩ and advected magnetic island ﹩(\delta {B}_{x}^{i}﹩, green curve) modes. Top-right panel: parallel (z) magnetic field fluctuations for forward (black curve) and backward (orange curve; ±) slow MS modes ﹩\delta {B}_{z}^{{s}^{\pm }}/{B}_{0}﹩. Middle-right panel: forward and backward transverse velocity fluctuations ﹩\delta {B}_{x,y}^{{s}^{\pm }}﹩ for slow MS modes. Bottom-right panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {B}_{y}^{{A}^{\pm }}﹩ and advected magnetic island ﹩(\delta {B}_{y}^{i}﹩, green curve) modes.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis of PSDs for the density fluctuations, consisting of entropy (black curve), fast (green curve) and slow (orange curve) MS modes (left column), velocity field fluctuations, consisting of Alfvén (blue curve), fast (green curve) and slow (orange curve) MS modes (middle column), and magnetic field fluctuation, consisting of magnetic islands (purple curve), Alfvén (blue curve), fast (green curve) and slow (orange curve) MS modes (right column) over eight 30 minute subintervals in fast solar wind.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis of the normalized velocity field fluctuations over the eight 30 minute subintervals within fast interval. Top-left panel: parallel (z) velocity component for forward (black curve) and backward (orange curve; ±) fast MS modes ﹩\delta {u}_{z}^{{f}^{\pm }}/{U}_{0}﹩. Middle-left two panels: forward and backward transverse velocity fluctuations ﹩\delta {u}_{x,y}^{{f}^{\pm }}﹩ for fast MS modes. Bottom-left panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {u}_{x}^{{A}^{\pm }}﹩ modes. Top-right panel: parallel (z−) velocity component for forward (black curve) and backward (orange curve; ±) slow MS modes ﹩\delta {u}_{z}^{{s}^{\pm }}/{U}_{0}﹩. Middle-right two panels: forward and backward transverse velocity fluctuations ﹩\delta {u}_{x,y}^{{s}^{\pm }}﹩ for slow MS modes. Bottom-right panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {u}_{y}^{{A}^{\pm }}﹩ modes.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis median energies for the density (green) fluctuations, consisting of entropy, fast and slow MS modes (left panel), velocity field (blue) fluctuations, consisting of Alfvén, fast, and slow MS modes (middle panel), and magnetic field (red) fluctuation, consisting of Alfvén, fast/slow MS modes, and magnetic islands modes (right panel), calculated over the frequency range (0.006–0.06)Hz corresponding to Alfvénic slow solar wind. The percentage values above each bar indicate the relative contribution of each mode of the total energy within its respective group.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Mode decomposition over a specific 30 minute Alfvénic slow solar wind interval showing density fluctuations from 03:45 to 04:15 on 2002 January 27. Top-left to -right: the frequency spectra for the entropy δρe (dashed black), forward fast (solid green) and slow (solid orange) δρfs+, and backward fast (dashed green) and slow (dashed orange) magnetosonic modes δρfs−, respectively. The bottom-left and -right panels depict similar spectra as in the top-left and -right panels, but in the wavenumber k-space.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis of the normalized density fluctuations over the eight 30 minute subintervals within fast solar wind. Top panel: normalized density fluctuations for the entropy modes. Middle panel: normalized density fluctuations for the forward (blue curve) and backward (orange curve) fast MS modes. Bottom panel: normalized density fluctuations for the forward (blue curve) and backward (orange curve) slow MS modes, where they overlap with each other. All fluctuating quantities are normalized to the mean density as labeled.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for the low-velocity channels in the CO line. Yellow and cyan dashed lines denote the eastern wall (P.A. ∼ −5°) and the western wall (P.A. ∼ −22°), respectively, of the northern lobe.
Paper: Explainable Machine Learning Classification of Chandra X-Ray Sources: SHAP Analysis of Multiwavelength Features
Authors: Shivam Kumaran, Samir Mandal, Sudip Bhattacharyya
Figure caption: Confusion matrix corresponding to the confused sources (CMP1 − CMP2 ≤ 0.05) in the identified dataset. The Y-axis shows the highest probable class, i.e., class 1 column in Table 1, and the X-axis is the second-highest probable class (class 2 column in Table 1).
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for CO. Yellow and cyan dashed lines denote the eastern wall (P.A. ∼ −5°) and the western wall (P.A. ∼ −22°), respectively, of the northern lobe.
Paper: Explainable Machine Learning Classification of Chandra X-Ray Sources: SHAP Analysis of Multiwavelength Features
Authors: Shivam Kumaran, Samir Mandal, Sudip Bhattacharyya
Figure caption: Location of the sources in Galactic coordinates belonging to different classes: AGN, stars (top-left); YSO, HMXB (top-right); CV, LMXB (bottom-left); pulsars, ULX (bottom-right) in Aitoff projection. Note: the pairs for the plot are selected for better visualization.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for H2CO32,2–22,1.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for H2CO30,3–20,2.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for SiO.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for SO.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Comparison between the optical/UV emission from 24puz, LFBOTs (A. Y. Q. Ho et al. 2023; Y. Yao et al. 2023; A. A. Chrimes et al. 2024b; M. Pursiainen et al. 2024), and TDEs (Y. Yao et al. 2023; J. J. Somalwar et al. 2025). In all panels, LFBOTs are shown in orange, TDEs are shown in blue, and 24puz in red. The left panel shows the blackbody luminosity evolution. Observational constraints are shown as points, whereas the lines show linear extrapolations between observations. In the case of TDEs, we show the compilation from J. J. Somalwar et al. (2025), who identified TDEs with published nonparametric blackbody luminosity modeling (T. W. S. Holoien et al. 2014, 2016; N. Blagorodnova et al. 2017, 2019; M. Nicholl et al. 2020; A. V. Payne et al. 2021; P. Charalampopoulos et al. 2023). We show the lightcurves relative to the first constraint, which is typically postpeak, explaining the relatively flat early time lightcurves. LFBOTs show rapid fading with a similar late-time power-law decay as 24puz, but on overall slower timescales and typically with fainter luminosities. TDEs show a range of lightcurve shapes, which generally evolve slower than that of 24puz. Some TDEs show a rapid fade like 24puz, but these are all at least 1 order of magnitude fainter than 24puz. These trends are highlighted in the right panel, which shows the peak g-band luminosity versus time above half-peak luminosity. We also include fast blue optical transients (FBOTs) as faint diamonds. TDEs are divided into featureless TDEs (F-TDEs, circles), which show featureless spectra like 24puz, and those that have transient spectral features (diamonds). 24puz is intermediate to LFBOTs and TDEs, and is notably more luminous than all events at a similar timescale and is much faster evolving than F-TDEs.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Left: star formation versus stellar mass of G1 relative to other galaxy populations. Constraints from the optical spectroscopy of G1 are shown in red. LFBOT hosts from D. A. Perley et al. (2019, 2021), D. L. Coppejans et al. (2020), A. A. Chrimes et al. (2024a), Y. Yao et al. (2022), and A. Y. Q. Ho et al. (2020) are shown in orange, and TDE hosts from Y. Yao et al. (2023) in blue. The core-collapse supernova host galaxy sample from S. Schulze et al. (2021) is shown in gray. Lines of constant specific star formation rate (sSFR) are shown in gray dashed. 24puz lies below the star-forming main sequence. Its location is consistent with LFBOT host galaxies, but is at a low sSFR and stellar mass relative to core-collapse supernova hosts and a low stellar mass relative to TDE hosts. Right: star formation versus physical offset from host galaxy of 24puz relative to other populations. The format is the same as in the left panel, except that we have colored the points by their stellar mass but left the marker outline colors the same as in the left panel. For TDEs, we assume a host galaxy offset ﹩\lt 0\mathop{.}\limits{^{\prime\prime} }6﹩. The LFBOT AT 2020xnd does not have a reported offset, so we assume that it is ≲1″, based on a by-eye approximation from images in D. A. Perley et al. (2021). 24puz is at a larger offset than expected from its host galaxy mass, if it is associated with a star-forming region.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: The evolution of the best-fit blackbody parameters to the optical/UV photometry of 24puz. The blackbody luminosity, radius, and temperature are shown in the top, middle, and bottom panels, respectively. The luminosity rapidly rises over a few days, then slowly rises/plateaus before rapidly decaying. The radius expands at a velocity of 0.1c or a power law ∼t0.4 and then decays as t−1.3 after a ∼week. The temperature is largely constant, and the weighted-mean value is ﹩\mathrm{log}{T}_{{\rm{bb}}}/{\rm{K}}=4.32\pm 0.14﹩.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Morphology of the nearest galaxy to 24puz, which we name G1. We show HST/WFC3 imaging of G1 in the F606W (left), F105W (middle), and F160W (right) bands. These images were taken 56 rest-day postdiscovery. We have reprojected all images to the F606W pixel scale for ease of comparison, but this means that the F105W and F160W have been resampled to a smaller pixel scale than the original images. G1 and 24puz are labeled. The white lines show contours, which highlight the morphology of G1. In all bands, there is an extended tidal tail or other irregular component toward the top left of G1. The contour levels are shown for visualization but are not intended to represent σ levels.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Fits to the absorption lines Fe II λλ2586, 2600, Mg II λλ2796, 2803, and Mg I λ2852. The spectra are fit as linear continuum components and Gaussian lines, as described in Section 4.1.1. The Gaussian widths and redshifts are fixed to the same value for all lines. The best-fit redshift is z = 0.35614 ± 0.00009. The Mg II absorption is consistent with a strong-absorber (EW2796 = 0.753 ± 0.104 Å > 0.3 Å), suggesting that this absorption is more likely occurring within the nearest galaxy to 24puz (G1) or a nearby group/cluster.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Emission line fits to the optical spectrum of 24puz from MJD 60590.2, or 61.4 rest-day postdiscovery. Fits to Hβ, Hα, and the [O II] λλ3726, 3729 doublet are shown in the left, middle, and right panels, respectively. The data is shown in black. The amplitudes of the Balmer lines are tied to the expected ratio for star formation, and the ratio of the [O II] doublet amplitudes are likewise tied. The apparent line at the location of Hβ is a sky subtraction artifact—rereducing the spectrum with different sky subtraction algorithms removes this feature. The [O II] line, on the other hand, is robust to sky subtraction. Blue lines show samples from our Gaussian emcee fits.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Constraints on the stellar population of G1. We assume a simple stellar population, due to a lack of constraints on the galaxy emission. The corner plot shows the distribution of possible stellar ages (tage), metallicities Z, and stellar masses M* with gray contours overlaid. The mass–metallicity relation from E. N. Kirby et al. (2013) is shown in dark purple. We find that G1 is a dwarf galaxy with M* ≲ 108.75 M⊙. If it lies on the mass–metallicity relation, then the mass is 107.75 ≲ M*/M⊙ ≲ 108.25, and the age tage/Myr ∼ 100 Myr.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Left: the MJD 60536 (21.4 rest-day) XMM-Newton spectrum of 24puz (blue scatter) with the best-fit power-law model overlaid. Right: corner plot showing the best-fit power-law parameters. The host galaxy absorption is negligible (nH ≲ 3 × 1021 cm−2). The power-law index is ﹩{\rm{\Gamma }}=1.7{3}_{-0.09}^{+0.10}﹩.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Position angle of the Keck I/LRIS longslit for each observation, overlaid on the HST/WFC3 F105W observation. 24puz is toward the bottom right corner of the image, whereas the galaxy is in the center. The MJD 60590 observation longslit was positioned to include the nearby galaxy and 24puz.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: The J0910b field. Left: SDSS composite image (g + r + i) with KCWI fields overlaid. Each pointing uses the Large Slicer configuration, with a field of view of 33″ × 20﹩\mathop{.}\limits^{\unicode{x02033}}﹩4. Two pointings, offset2 and offset3, cover one side of the circumgalactic medium (CGM) extending in the SE direction out to ∼50″ (∼90 kpc), corresponding to ∼0.9 Rvir of J0910b’s halo. Photometric galaxies are labeled with their photometric redshifts (PhotoZ), where available; they are foreground or background systems unrelated to J0910b. Right: white-band image (∼270 Å near Hα) of J0910b from KCWI-red, alongside spectra extracted from the central 10 × 10 spatial pixels (spaxels). The KCWI-blue spectrum (blue) and KCWI-red spectrum (red) highlight differences in spectral resolution, with 〈R〉 ∼ 900 for KCWI-blue and 〈R〉 ∼ 1400 for KCWI-red. Galactic extinction has been corrected using E(B − V) = 0.0389 (see Appendix A).