adsabs/AstroCLIMB huggingface dataset:
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the peak brightness and flux density for sources imaged in the BJ083 and UD001 sessions. Top panel: (a) distribution of the image peak brightness, S p, and (b) the total CLEAN flux density, ﹩{S}_{\mathrm{cln}}﹩, taken from the last epoch that each source was observed at. Bottom panel: (c) distribution of the median correlated flux density computed over the shortest baselines, S s, and (d) over the longest baselines, S l, taken from the last epoch that each source was observed at. The mean and median values are shown in the top right corner of each plot.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the peak brightness and flux density variability indices for sources imaged in the BJ083 and UD001 sessions. Top panel: (a) distribution of the variability indices of the image peak brightness, S p, (b) the core flux density, S c, and (c) the total CLEAN flux density, ﹩{S}_{\mathrm{cln}}﹩, for sources observed in more than one epoch. Bottom panel: (d) distribution of the variability indices of the correlated flux densities over the shortest baselines, S s, and (e) the longest baselines, S l, for sources observed in more than one epoch. The mean and median values are given in the top-right corner.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: (a) Distribution of the median source structure delay corrections, τ median, and (b) distribution of the corresponding structure index, SI, taken from the last epoch that each of the sources was observed at. (c) Distribution of the per-source standard deviations of the structure index, σ SI, for sources observed in more than one epoch. The mean and median values are given in the top-right corner.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Selection of images of J0423−0120 (IVS B0420−014), with (a) the J0423−0120 image from BJ083B, (b) the image from UD001C, and (c) the image from UD001J.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the image quality factor taken over all 5879 images from the BJ083 and UD001 sessions. The mean and median values are shown in the top-right corner.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Selection of images from sources that show significant structure. Top panel: (a) image of J0403+2600 (IVS B0400+258) from session UD001H, and (b) image of J0006−0623 (IVS B0003−066) from session BJ083B, and (c) image of J1242+3720 (IVS B1239+376) from session UD001H. Bottom panel: (d) image of J1550+0527 (IVS B1548+056) from session BJ083C, and (e) image of J0432+4138 (3C 119) from session UD001C, and (f) image of J1744−3116 (IVS B1741−312) from session UD001W.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the DIFMAP, model-fit estimates of (a) the FWHM angular size of the core component, (b) the FWHM angular size of the second component, and (c) the radius of the second component from the phase center, for all of the images from the BJ083 and UD001 sessions. The mean and median values are given in the top-right corner.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Selection of images of J2230+6946 (IVS B2229+695), with (a) the J2230+6946 image from BJ083C, (b) the image from BJ083D, and (c) the image from UD001J.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Image (a) of J0221+355A (IVS B0218+357) from session UD001C, and (b) from session UD001L.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: Diagrams of the PMM against parallaxes showing the box defined to select kinematic members (solid black lines). The gray dots indicate GAIA sources with good astrometric quality (see Section 2.2.1), and blue symbols indicate the subsample observed by LAMOST.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: LAMOST fields in the OSFC. We combine a dust infrared emission map (Schlegel et al. 1998; green map) and an Hα emission map (Finkbeiner 2003; red map). We also show isocontours of the CO map of Dame et al. (2001) and the region of the Orion OB1b subassociation defined by (Briceño et al. 2019; yellow dashed lines), which include stars in the Orion belt (large white stars). As a reference, we include the location of O-type stars (yellow circles) and B-type stars earlier than B3 (cyan circles), compiled by Anderson & Francis (2012). The LAMOST fields are located mostly in the general region of the Orion OB1a subassociation.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: Color–magnitude diagrams for PMS candidates in the three LAMOST fields. We plot the straight line V = 2.7 × [V– J] + 10.15 to select stars above the MS (solid red lines). As a reference, we also plot PARSEC isochrones (Marigo et al. 2017) at 30 Myr (solid black line) and 1 Myr (dashed black line). More than 40% of the PMS candidates are located below the 30 Myr isochrone.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: The upper-left panel shows a color–absolute magnitude diagram (not corrected for reddening) of the bona fide TTSs (blue circles) and the kinematic members (K_MEM*) selected in a large area that includes the three LAMOST fields (gray circles in the lower panels). We define a sample of kinematic TTS candidates (black dots) selecting stars with [Bp – Rp] > 1.0 that fall above the line traced by the function Y = 2.6 + 2.1 × X. The red dashed lines represent this function and the [Bp – Rp] limit. The upper-right panel shows the distribution of distances (1000/Π C ) for the kinematic TTS sample. We also plot the distance distribution of the four kinematic groups detected in Section 3.3. These distributions were multiplied by 10 to provide a better comparison with the kinematic TTS candidates. This distribution has a minimal value at 385 pc (black dashed line), suggesting two stellar populations separated in distance. The lower panels show numerical density maps of the kinematic TTS candidates located closer than 385 pc (left panel) and farther than 385 pc (right panel). We plot the spatial distributions of the four kinematic groups detected in the bona fide TTS sample. To avoid highly clustered stellar populations (e.g., ONC and σOri), we reject stars below the solid line (decl. = 1.5 × R.A. – 129°).
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: SEDS of the bona fide TTS sample with available WISE photometry, ordered by spectral type. We include GAIA (yellow diamonds), 2MASS (green circles), and WISE (red squares) photometry, normalized to the H band, and dereddened using the A  V  values in Table 3, and adopting the extinction law of Cardelli et al. (1989) with R  V  = 3.1 for the GAIA and 2MASS photometry, and the extinction law of Wang & Chen (2019) for the WISE photometry. Error bars are included for the W3 and W4 photometry; the errors are smaller than the symbols for the rest of the photometry. The gray solid zone represents the stellar photosphere, including the uncertainty in spectral type. We include the Spitzer/InfraRed Spectrograph (IRS) Taurus median from Furlan et al. (2006), constructed from disks around stars with K5–M2 spectral types (solid black line). The shaded region represents the quartiles of the flux distribution.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: H-R diagram showing the bona fide TTS sample with RUWE < 1.0 (magenta filled circle) and RUWE between 1.0 and 1.4 (blue open circles). We also plot stars with an uncertain kinematic status and Li I detected (fl_Li = 2; green open circle), highlighting stars with a fidelity < 0.5 (yellow filled circle). As a reference, we plot the 5 and 10 Myr isochrones (Marigo et al. 2017) and the corresponding equal mass isochrones.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: Infrared WISE color–color diagrams. The left and middle panels show the distribution of the bona fide stars in the south and north fields, respectively. The accretion classes defined in Section 3.1 are indicated with different symbols and colors. The open symbols indicates stars with an S/N in 22 μm photometry between 2 and 3 (photometric quality “C”). The empirical loci for different disk types were estimated using the infrared colors of the disk populations in Upper Sco and Taurus (Luhman & Mamajek 2012; Esplin et al. 2014; Thanathibodee et al. 2022). The solid box represents the locus for full disks. Transitional disks are expected to fall below the solid black line. The loci for evolved disks, debris disks, and diskless stars are represented with black, gray, and light gray dashed boxes, respectively. The right panel shows the synthetic WISE colors estimated using a grid of irradiated accretion disk models with a 0.5 M ⊙ central star. Different symbols represent different degrees of dust settling. The accretion rates are represented by different sizes (5 × 10−10, 1 × 10−9, 5 × 10−9, 1 × 10−8, and 2 × 10−8 M ⊙ yr−1) The color bar represents different disk inclinations, where smaller values indicate more edge-on disks (see the text for details).
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: Upper panels: identified stellar kinematic groups using the HDBSCAN clustering algorithm. The left panel shows the two kinematic groups detected in the south field, South_Near (orange circles) and South_Far (blue circles). The right panel shows the two kinematic groups detected in the north fields, North_Near (orange circles) and North_Far (blue circles). The gray circles show stars not assigned to a kinematic group. Lower panels: membership regions of stellar clusters identified with HDBSCAN from the bona fide TTS sample for each field; (left) corresponds to the south and (right) corresponds to the north. The boxes represent the membership cube defined using the MAD and 3σ criterion in Π C , μ  α , and μ  δ .
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: Comparison of the effective temperatures determined in this work with previously published values. We use the conversion table from Pecaut & Mamajek (2013) to obtain the effective temperatures of the spectral types defined in Briceno (2008) and in Section 3.1. Gray crosses and open black triangles represent stars with effective temperatures obtained from Briceño et al. (2019) and APOGEE Net (Sprague et al. 2022), respectively. The open circles show the effective temperatures derived by GAIA-Apsis (Creevey et al. 2022), in which the color represents different extinctions obtained with this tool. Stars with the highest extinctions estimated by GAIA-DR3 show the larger discrepancies, suggesting a temperature–extinction degeneracy during the estimation of the GAIA-DR3 stellar parameters.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: H-R diagrams. The upper panels include stars with a reliable detection of Li I, while the lower panels include stars with doubtful or no Li I detection. The left and right panels show the locations of stars in the south and north fields, respectively. The different colors represent different kinematic classes. For reference, we include the 1, 5, 10, 50, and 1000 Myr isochrones from PARSEC (Marigo et al. 2017).
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: The left panel shows a spatial distribution of the bona fide TTS sample representing each kinematic group with different colors. The gray circles represent the LAMOST fields. The dashed circle shows the limits of the Orion OB1b subassociation (Briceño et al. 2019). The right panels shows histograms of the stellar age for the four kinematic groups estimated using PARSEC models (Marigo et al. 2017) and MIST models (Dotter 2016). We multiply the histograms of the north fields by two to obtain a better visual comparison with the south field.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: Logarithm of the EW of H α  as a function of spectral type of stars with spectral types K or M with flag_Li I > 0. We have classified these stars into CTTSs (red symbols), WTTSs (green symbols), and CWTTSs (blue symbols), following Briceño et al. (2019). The dashed line indicates the upper limit for WTTSs, while the dotted line indicates the lower limits for CTTSs. The solid symbols indicate bona fide TTS stars.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: RUWE vs. fidelity_v2. Only two stars, labeled in the plot, have a good astrometric solution using the RUWE and a bad astrometric solution from the fidelity criterion. In contrast, a significant number of stars have a good astrometric solution from the fidelity criterion but are classified with a bad astrometric solution using the RUWE.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: Diagrams comparing the masses and ages estimated from two evolutionary models. The left panel compares the stellar masses derived using the PARSEC and MIST models. We highlight the bona fide TTS sample in which the color bar indicates the age derived using the PARSEC models. The right panel compares the ages derived using the PARSEC and MIST models. In this case, the color bar represents the stellar mass estimated from the PARSEC models for the bona fide TTS sample. Stars not included as bona fide TTSs are plotted with an X.
Paper: A LAMOST Spectroscopic Study of T Tauri Stars in the Orion OB1a Subassociation
Authors: Jesús Hernández, Luisa F. Zamudio, César Briceño, Nuria Calvet, Zhaohuan Zhu, Haibo Yuan, Xiaowei Liu, Ezequiel Manzo-Martínez, Carlos G. Román-Zúñiga, Javier Serna, Karina Maucó, Lucía Adame
Figure caption: H-R diagrams for the North_Near (upper-left panel), North_Far (upper-right panel), South_Near (lower-left panel), and South_Far (lower-right panel) kinematic stellar groups. Different colors and symbols represent different accretion classes defined following the classification scheme of Briceño et al. (2019).
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Moment one velocity maps from WSRT imaging, with WSRT H I column density contours superimposed in dark gray, for (from top to bottom) AGC 123216, AGC 219369, AGC 229398, and AGC 333576, and their nearby potential parent galaxies. The left panels show the full field around each AD, and the right panels show a close-up of the AD. Beam size is shown as a shaded gray ellipse. The figures for AGC 123216, AGC 219369, and AGC 333576 have column density contours at N H I  = (0.1, 0.5, 1.2, 2.4, 4.5) × 1020 cm−2, while the figures for AGC 229398 have contours at N H I  = (0.1, 0.2, 0.4, 0.8, 1.6) × 1020 cm−2, where the lowest contours are the first listed. Note that KUG 1158+216 is not included in the full-field map for AGC 229398 because we did not have WSRT H I maps for it.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Position–velocity slices of 1 pixel width along the major-axis from the best-fitting model of each AD-TDG candidate, from WSRT data. The data are shown in gray, with white contours at 2, 4, 8, and 16 times the S/N of the data. Dashed dark gray contours represent −2 × S/N. The red contours represent the best-fit model, and the yellow points mark the line-of-sight rotation velocities from the model.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image showing the full-field view of AGC 219369 (bottom), including potential parent NGC 3510 (top). There are WSRT H I column density contours at N H I  = (0.1, 0.5, 1.2, 2.4, 4.5) × 1020 cm−2 superimposed in white. The physical scale bar is calculated for a distance of 9.2 Mpc.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Masking, surface brightness profiles, and profile fit parameters for AGC 123216 in ﹩g^{\prime} ﹩ (top row of each panel) and ﹩r^{\prime} ﹩ (bottom row of each panel), with optical images from the WIYN 3.5 m telescope. For each object, the left images show the original image with a small red x marking the optical center; the center images show the ellipses that were placed in red and pixels that were masked in green, based on the masking procedure described in Section 3.4; and the right images show the best-fitting surface brightness profile, along with the uncertainty shaded in light gray and the parameters for that fit listed below. For AGC 123216, there were no pixels flagged for masking in either filter.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite images of NGC 807. Left: Color image revealing low-surface-brightness, dusty spiral arms surrounding a large and bright bulge. The image has been scaled to show the full extent of the faint disk, which overemphasizes the bulge at the center. Right: Composite ﹩g^{\prime} +r^{\prime} ﹩-band summed image in inverted grayscale showing arms of stellar emission extending in several directions, primarily out of the northern edge of the disk. The image has been binned 3x3 to make the arms easier to see. Note that this image is a different scale than the left panel, as the region of the disk in that image is the entire black area here.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image showing the full-field view of AGC 123216 (center) with potential parents NGC 807 (top), MRK 365 (bottom right), and MCG 05-06-003 (bottom left). There are WSRT H I column density contours at N H I  = (0.1, 0.5, 1.2, 2.4, 4.5) × 1020 cm−2 superimposed in white.