adsabs/AstroCLIMB huggingface dataset:
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program): The Magnetic Fields in the Multiphase Interstellar Medium of the Antennae Galaxies 
Authors: Enrique Lopez-Rodriguez, Alejandro S. Borlaff, Rainer Beck, William T. Reach, Sui Ann Mao, Evangelia Ntormousi, Konstantinos Tassis, Sergio Martin-Alvarez, Susan E. Clark, Daniel A. Dale, Ignacio del Moral-Castro
Figure caption: Comparison of the B-field orientation at 154 μm with the multiphase ISM. The B-field orientations at 154 μm (white lines) over the 12CO(1–0) (top left) and H I (top middle) emission lines; H α  (top right), 12CO(1–0) (middle left), and H I (middle) velocity dispersion; X-ray (middle right); mask (bottom left); ﹩{N}_{{\rm{H}}\,{\rm\small{I}}+{{\rm{H}}}_{2}}﹩ (bottom middle); and T d (bottom right) are shown. We display the same B-field orientation as shown in Figure 2. The contours in ﹩{N}_{{\rm{H}}\,{\rm\small{I}}+{{\rm{H}}}_{2}}﹩ start at ﹩{\mathrm{log}}_{10}({N}_{{\rm{H}}\,{\rm\small{I}}+{{\rm{H}}}_{2}}[{\mathrm{cm}}^{-2}])=18﹩ and increase in steps of 0.2. The contours in T d start at 20 K and increase in steps of 0.5 K. The contours in the 12CO(1–0) and H I velocity dispersion start at 10 km s−1 and increase in steps of 10 km s−1. The beam size (red circle) of the 154 μm observations is shown.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program): The Magnetic Fields in the Multiphase Interstellar Medium of the Antennae Galaxies 
Authors: Enrique Lopez-Rodriguez, Alejandro S. Borlaff, Rainer Beck, William T. Reach, Sui Ann Mao, Evangelia Ntormousi, Konstantinos Tassis, Sergio Martin-Alvarez, Susan E. Clark, Daniel A. Dale, Ignacio del Moral-Castro
Figure caption:  B-field orientations in the plane of the sky (streamlines) at wavelengths of 154 μm (left) and 11 cm (right; Basu et al. 2017, corrected for Faraday rotation) over a color image of the Antennae galaxies. The color image was computed using HST F435W (blue), F550M (green), and a combination of F814W and F658N (red) by Whitmore et al. (2010). The inferred B-field orientation at 154 μm is shown as streamlines using the Line Integral Convolution (Cabral & Leedom 1993) technique (resample = 20). At 154 μm, we show polarization measurements with I/σ  I   ≥  100, PI/σ PI  ≥  3, and P  ≤  20%, where σ  I  and σ PI are the uncertainties in the total and polarized intensities, respectively. At 11 cm, we show polarization measurements with PI/σ PI  ≥  5. We show the labels of the regions studied in this work and the beam size (white circle) of the 154 μm observations.
Paper: Finding Peas in the Early Universe with JWST
Authors: James E. Rhoads, Isak G. B. Wold, Santosh Harish, Keunho J. Kim, John Pharo, Sangeeta Malhotra, Austen Gabrielpillai, Tianxing Jiang, Huan Yang
Figure caption: The emission lines and fits to these lines for objects in our analysis are shown here. The four panels correspond to J072326–732656 (04590) (top left), J072322–732606 (06355) (bottom left), J072320–732604 (10612) (bottom right), and two SDSS Green Pea spectra (top right). All spectra display rest wavelength and flux density f  λ  (scaled to render lines easily visible). Within each of the JWST panels, the upper and lower rows of subpanels correspond to the two distinct NIRSpec exposures. For the Green Pea panel, the upper and lower subpanels correspond to two distinct objects. Within each row, four distinct wavelength segments are plotted. Each segment shows a linked line set, where we performed a joint fit to two to four emission lines. Each fit included three parameters to describe the redshift, line width, and continuum level, plus one parameter per emission line to measure line amplitudes. The four fitted line sets are (from blue to red) [O II] 3727, 3729 + [Ne III] 3869 + Hζ 3890; [Ne III] 3968 + Hϵ 3971 + Hδ 4102; Hγ 4341 + [O III] 4364; and Hβ 4862 + [O III] 4960 + [O III] 5008.
Paper: Finding Peas in the Early Universe with JWST
Authors: James E. Rhoads, Isak G. B. Wold, Santosh Harish, Keunho J. Kim, John Pharo, Sangeeta Malhotra, Austen Gabrielpillai, Tianxing Jiang, Huan Yang
Figure caption: Comparison of the rest-optical spectra of the Green Pea galaxies J1220 + 4915 (z = 0.012) and J0827 + 3429 (z = 0.085), and the Epoch-of-Reionization galaxies J072326–732656 (04590), J072322–732606 (06355), and J072320–732604 (10612). The Green Pea galaxies shown are selected as the two best analogs to the line ratios of J072326–732656 (04590) among the Green Pea sample from Yang et al. (2019) and Jiang et al. (2019; see Section 2.4). For display purposes we have masked a few spurious features in these early-release JWST spectra that did not match any known spectral line, after confirming that these features were not consistently present in both exposures.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program): The Magnetic Fields in the Multiphase Interstellar Medium of the Antennae Galaxies 
Authors: Enrique Lopez-Rodriguez, Alejandro S. Borlaff, Rainer Beck, William T. Reach, Sui Ann Mao, Evangelia Ntormousi, Konstantinos Tassis, Sergio Martin-Alvarez, Susan E. Clark, Daniel A. Dale, Ignacio del Moral-Castro
Figure caption: Comparison of the polarization measurements between radio and FIR wavelengths for the different regions studied. Left: the histograms of P (top) in 0.5% bins and the B-field orientation in bins of 10° at 154 μm (middle) and 11 cm (bottom) are shown. The median and 1σ uncertainties are shown. Right: median 154 μm P (top), the slopes (Figure 4) of the P–T d (middle) and ﹩P\mbox{--}{N}_{{\rm{H}}\,{\rm\small{I}}+{{\rm{H}}}_{2}}﹩ (bottom) of the Antennae’s regions, and for spiral (M51, M83, NGC 3627, NGC 4736, NGC 6946, and NGC 7331) and starburst (M82, NGC 253, and NGC 2146) galaxies at 154 μm taken from Lopez-Rodriguez et al. (2022b) are shown.
Paper: Finding Peas in the Early Universe with JWST
Authors: James E. Rhoads, Isak G. B. Wold, Santosh Harish, Keunho J. Kim, John Pharo, Sangeeta Malhotra, Austen Gabrielpillai, Tianxing Jiang, Huan Yang
Figure caption: This figure, based on Figure 8 of Jiang et al. (2019), shows the relation between R 23, O 32, and gas-phase metallicity. Black points mark the Green Pea galaxies used to derive the plotted contours, which are labeled with corresponding values of ﹩12+\mathrm{log}[{\rm{O}}/{\rm{H}}]﹩. Gray ovals mark 1σ uncertainty regions for the three z > 7 objects, which have inferred R 23 metallicities of ∼7.3 (J072326–732656 (04590)), ∼8.3 (J072322–732606 (06355)), and ∼8.3 (J072320–732604 (10612)). The first two measurements are in good agreement with the T  e  method results, while J072320–732604 (10612) appears to be an outlier in this relation. Together, this trio of sources spans the range of R 23 seen in the comparison sample of Green Pea galaxies.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program): The Magnetic Fields in the Multiphase Interstellar Medium of the Antennae Galaxies 
Authors: Enrique Lopez-Rodriguez, Alejandro S. Borlaff, Rainer Beck, William T. Reach, Sui Ann Mao, Evangelia Ntormousi, Konstantinos Tassis, Sergio Martin-Alvarez, Susan E. Clark, Daniel A. Dale, Ignacio del Moral-Castro
Figure caption: Polarization measurements vs. dust temperature and column density for three regions: relic spiral arm, overlap region, and tidal tail. The I (top), PI (middle), and P (bottom) vs. T d (left) and ﹩{N}_{{\rm{H}}\,{\rm\small{I}}+{{\rm{H}}}_{2}}﹩ (middle and right) at 154 μm (left and middle) and 11 cm (right) are shown. The best-fit model and the slopes with their uncertainties for each region are shown in each panel.
Paper: The Identification of a Dusty Multiarm Spiral Galaxy at z = 3.06 with JWST and ALMA
Authors: Yunjing Wu, Zheng Cai, Fengwu Sun, Fuyan Bian, Xiaojing Lin, Zihao Li, Mingyu Li, Franz E. Bauer, Eiichi Egami, Xiaohui Fan, Jorge González-López, Jianan Li, Feige Wang, Jinyi Yang, Shiwu Zhang, Siwei Zou
Figure caption: Dusty spiral galaxy (DSG) at z = 3.059. The composite RGB map of the target A2744-DSG-z3 is based on 3-band JWST/NIRISS imaging observations with pixel scale of 0.″03 (blue: F115W, green: F150W, red: F200W). The target A2744-DSG-z3 was initially reported by the ALMA Frontier Fields survey (González-López et al. 2017; Laporte et al. 2017, A2744-ID03 in their papers) as an SMG (see also Sun et al. 2022). Meanwhile, the target GLASS-Z grad1, reported in Wang et al. (2022), is a star-forming galaxy with stellar mass (M *) of ∼109 M ⊙ at the same redshift. The impact parameter between these two galaxies is ≈3.″1. Another emission-line galaxy is confirmed by NIRISS grism and ALMA as well at z = 3.05 (M. Li et al. 2022, in preparation) with the projected separation of 15″. This galaxy was also reported as an SMG with M dust ≃ 108.6 M ⊙ (Laporte et al. 2017; Sun et al. 2022).
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: Stellar population properties of the JWST counterparts of the ALMA sources. The two multiply imaged systems EG-ALMA 2a/2b, EG- ALMA 6a/6b/6 c and the point source UDS-ALMA 2 are excluded. Left: star formation rate versus stellar mass. All values have been corrected for magnification. The points with error bars represent the 13 galaxies, and the lines show the star formation main sequence (Speagle et al. 2014). The points and lines are color coded by redshift as labeled and indicated in the legend. Middle: ratios of the specific star formation rates of our sources to those of the main sequence galaxies as a function of redshift. The colored points with error bars are the 13 ALMA sources, and the open circles show the SMGs from the AS2UDS program (Dudzevičiūtė et al. 2020) for comparison. The dashed horizontal lines (ratios of 1/4 and 4, respectively) indicate the nominal range within which galaxies are considered to be on the main sequence. Right: UVJ color–color diagram. The points represent the ALMA-source host galaxies, color coded by their sSFR/sSFRms values as indicated by the color bar to the right. The rest-frame UVJ colors were computed by EAZY from the best-fit templates at the adopted redshifts. The cross in the lower right corner indicates our estimate of the typical uncertainties. The black open circles show the UVJ colors of the AS2UDS SMGs (Stach et al. 2019) for comparison. The quiescent-galaxy region marked by solid lines in the upper left is based on Patel et al. (2012). The one blue data point in this region is TN-ALMA 2 (z phot  =  2.79). Its reddest passband, F360M, does not reach the rest-frame J band, and therefore EAZY's estimate of its V − J color has large uncertainty.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: (a) Images of the ALMA sources in El Gordo, one source in each row. Each stamp is 5″ × 5″ in size. Both the archival HST ACS images (F850LP or F814W) and the new JWST NIRCam images (F090W to F444W) are shown with bandpass filters noted at top. The ALMA Band 6 (1.1 mm) contours (2σ in blue; 3, 5, and 10σ in red) are superposed on the F356W images, and the Band 7 (870 μm) contours when available are superposed on the F444W images (using the same contour color-coding as for Band 6). The ALMA beams are shown as the red-filled ellipses. (b) Images of the ALMA sources in UDS. The images are 5″ × 5″ in size. (c) Images of the ALMA sources in TNJ1338. The images are 10″ × 10″ in size.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: Results of EAZY fitting to derive z phot independently. Points show observed data, and solid lines show the best-fit templates. Best-fit redshift is indicated in each panel. Insets show the redshift probability distributions. For UDS-ALMA 3, z spec  =  1.089 and for UDS-ALMA 5, z spec  =  2.154, which are both in excellent agreement with the photometric redshift estimates from EAZY listed in their figure panels. UDS-ALMA 2 is fitted using the AGN templates, and the best-fit template is the obscured AGN A2690#75 from Fiore et al. (2008). The vertical scales of all panels cover a 7 mag range, though with differing offsets, to allow comparison of the SEDs.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: SED-fitting results using MAGPHYS-PHOTOZ. The legend in each panel gives the z spec value when available. The red dots show the observed data, and the thick black lines show the best-fit templates. The multiply imaged systems EG-ALMA 2a/2b and EG-ALMA 6a/6b/6 c suffer from unreliable photometry because of the lensing distortion, and therefore the fits for individual images for the individual images have large error bars. UDS-ALMA 2 is a point source and very likely a quasar, and therefore the stellar templates used by MAGPHYS-PHOTOZ might not be applicable. It is still shown here for completeness. We note that the photometric redshifts and uncertainties agree well with the spectroscopic redshifts when these are available.
Paper: UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation
Authors: Michael J. Koss, Ezequiel Treister, Darshan Kakkad, J. Andrew Casey-Clyde, Taiki Kawamuro, Jonathan Williams, Adi Foord, Benny Trakhtenbrot, Franz E. Bauer, George C. Privon, Claudio Ricci, Richard Mushotzky, Loreto Barcos-Munoz, Laura Blecha, Thomas Connor, Fiona Harrison, Tingting Liu, Macon Magno, Chiara M. F. Mingarelli, Francisco Muller-Sanchez, Kyuseok Oh, T. Taro Shimizu, Krista Lynne Smith, Daniel Stern, Miguel Parra Tello, C. Megan Urry
Figure caption: Top left and middle: VLT/MUSE AO-assisted, 1″ wide map of ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]﹩ equivalent width and velocity in the heart of UGC 4211 scaled with linear stretch. Dashed circles mark the circular apertures used for 1D spectral extractions (0.″15 diameter) for the northern nucleus (N; blue), the southern nucleus (S; red), and the region halfway between them (M; green). For the velocity map, Voronoi binning was used to increase S/N to measure the ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]\,\lambda 5007﹩ emission line velocity offset (from z = 0.03474), with excluded low S/N regions in black. The positions of the two NIR nuclei are shown with blue crosses. Top right: ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]\,\lambda 5007﹩/Hβ map. Since Hβ is too weak for detection, we used the Hα emission, assuming a ratio of ∼15 as measured in the Hα/Hβ emission from the three spatial regions, with low S/N regions in black. Second row: spectra of the three spatial regions (north, south, middle), showing the key emission lines (i.e., Hβ, ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]﹩, Hα, [N II], ﹩\left[{\rm{S}}\,{\rm\small{II}}\right]﹩) along with the Ca II λ8498, 8542, 8662 absorption. Bottom row: strong line ratios Baldwin, Phillips, and Terlevich (BPT) diagrams for the three regions. Gray shaded contours denote the SDSS sample density (Oh et al. 2011).
Paper: UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation
Authors: Michael J. Koss, Ezequiel Treister, Darshan Kakkad, J. Andrew Casey-Clyde, Taiki Kawamuro, Jonathan Williams, Adi Foord, Benny Trakhtenbrot, Franz E. Bauer, George C. Privon, Claudio Ricci, Richard Mushotzky, Loreto Barcos-Munoz, Laura Blecha, Thomas Connor, Fiona Harrison, Tingting Liu, Macon Magno, Chiara M. F. Mingarelli, Francisco Muller-Sanchez, Kyuseok Oh, T. Taro Shimizu, Krista Lynne Smith, Daniel Stern, Miguel Parra Tello, C. Megan Urry
Figure caption: Multiwavelength, multiscale images of UGC 4211. Top left: 3′-wide grz color image from the DECaLS with an asinh stretch. The purple square indicates the 6″ zoom region used for the upper right panel, while the tiny red square is the 1″ zoom region used for our highest-resolution analysis of the dual nuclei. Top right: 6″ grz color image constructed from our new MUSE AO data cube. Here the red square indicates the 1″ zoomed-in circumnuclear region. The panels in the second row show the 1″ circumnuclear region in HST F814W (left), NIRC2 AO J-band (middle), and NIRC2 AO ﹩K^{\prime} ﹩ (right) in log stretch. The northern and southern emission components identified in NIR are indicated (N and S, respectively), and are separated by 0.″32, almost exactly along the north–south direction (PA 7.°5 of north). The panels in the bottom row show emission maps from our MUSE AO data, centered on ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]﹩ (left) and Hα (middle), as well as from ALMA continuum emission at ∼230 GHz (right, white hatched circle indicates the beam size.). The positions of the two NIR nuclei are shown with blue crosses.
Paper: UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation
Authors: Michael J. Koss, Ezequiel Treister, Darshan Kakkad, J. Andrew Casey-Clyde, Taiki Kawamuro, Jonathan Williams, Adi Foord, Benny Trakhtenbrot, Franz E. Bauer, George C. Privon, Claudio Ricci, Richard Mushotzky, Loreto Barcos-Munoz, Laura Blecha, Thomas Connor, Fiona Harrison, Tingting Liu, Macon Magno, Chiara M. F. Mingarelli, Francisco Muller-Sanchez, Kyuseok Oh, T. Taro Shimizu, Krista Lynne Smith, Daniel Stern, Miguel Parra Tello, C. Megan Urry
Figure caption: Estimate of the future SMBH pair semimajor axis evolution for UGC 4211 as a function of the semimajor axis. At its current separation (dotted line), UGC 4211 is likely nearing the end of its dynamical friction phase (DF, orange region). Once it forms a hard binary at a Hard (dashed line) its evolution will be driven by stellar hardening (SH, yellow region), then gas (green region), and finally gravitational waves (GW, blue region) until coalescence. They light gray region shows the semimajor axis scale where UGC 4211 will emit ∼nHz GWs.
Paper: UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation
Authors: Michael J. Koss, Ezequiel Treister, Darshan Kakkad, J. Andrew Casey-Clyde, Taiki Kawamuro, Jonathan Williams, Adi Foord, Benny Trakhtenbrot, Franz E. Bauer, George C. Privon, Claudio Ricci, Richard Mushotzky, Loreto Barcos-Munoz, Laura Blecha, Thomas Connor, Fiona Harrison, Tingting Liu, Macon Magno, Chiara M. F. Mingarelli, Francisco Muller-Sanchez, Kyuseok Oh, T. Taro Shimizu, Krista Lynne Smith, Daniel Stern, Miguel Parra Tello, C. Megan Urry
Figure caption: HST/STIS spatially resolved 2D spectroscopy of the ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]﹩ (top row) and the Hα spectral region (middle row). The spectroscopy is from a 0.″2 long slit, aligned with the two NIR nuclei in the N–S direction. The vertical axis is spatial (north–south) and the horizontal axis is spectral (λ increasing to the right). Bottom row: STIS spectra of the northern and southern sources in the ﹩\left[{\rm{O}}\,{\rm\small{III}}\right]﹩ and Hα spectral regions (extracted from 0.″2 wide apertures; first two panels), along with OSIRIS NIR spectra of the two nuclei (extracted from 0.″3 diameter aperture; last three panels).
Paper: UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation
Authors: Michael J. Koss, Ezequiel Treister, Darshan Kakkad, J. Andrew Casey-Clyde, Taiki Kawamuro, Jonathan Williams, Adi Foord, Benny Trakhtenbrot, Franz E. Bauer, George C. Privon, Claudio Ricci, Richard Mushotzky, Loreto Barcos-Munoz, Laura Blecha, Thomas Connor, Fiona Harrison, Tingting Liu, Macon Magno, Chiara M. F. Mingarelli, Francisco Muller-Sanchez, Kyuseok Oh, T. Taro Shimizu, Krista Lynne Smith, Daniel Stern, Miguel Parra Tello, C. Megan Urry
Figure caption: Left: VLT/MUSE AO-assisted, 1″ wide map of velocity from fitting the CaT stellar absorption region (8300–8900 Å) in the heart of UGC 4211 scaled with linear stretch. Voronoi binning was used to increase the S/N, with excluded low S/N regions in black. The positions of the two ALMA continuum sources (which closely match the NIR nuclei) are shown with white crosses. Right: ALMA 12CO(2-1) 1″ wide map showing the distribution of molecular gas velocities. Purple contours indicate the location of the velocity-integrated 12CO(2-1) emission. The white hatched circle shows the beam size.
Paper: UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation
Authors: Michael J. Koss, Ezequiel Treister, Darshan Kakkad, J. Andrew Casey-Clyde, Taiki Kawamuro, Jonathan Williams, Adi Foord, Benny Trakhtenbrot, Franz E. Bauer, George C. Privon, Claudio Ricci, Richard Mushotzky, Loreto Barcos-Munoz, Laura Blecha, Thomas Connor, Fiona Harrison, Tingting Liu, Macon Magno, Chiara M. F. Mingarelli, Francisco Muller-Sanchez, Kyuseok Oh, T. Taro Shimizu, Krista Lynne Smith, Daniel Stern, Miguel Parra Tello, C. Megan Urry
Figure caption: NIRC2 AO ﹩{K}^{{\prime} }﹩ 4″ image of UGC 4211 in log stretch overlaid with Chandra 3–7 keV (light blue) emission and 22 Ghz VLA emission (green). In Chandra, contours represent 5, 10, and 30 counts, respectively. The green hatched circle indicates the VLA beam size. The positions of the two NIR nuclei are shown with blue crosses. For both Chandra (FWHM ∼ 0.″5) and the VLA (∼1″) the resolution is insufficient to resolve the two sources. The offset of Chandra is likely due to astrometric errors in the alignment of the images (∼0.″3), even after using Gaia as a reference.