adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: A comparison of the emission line-based and kinematically derived gas disk masses. Kinematic gas mass upper limits are shown in gray. Blue lines show where line-based gas mass is 0.33×, 1×, and 3× the kinematically derived gas mass.
Paper: exoALMA. XIII. Gas Masses from N2H+ and C18O: A Comparison of Measurement Techniques for Protoplanetary Gas Disk Masses
Authors: Leon Trapman, Cristiano Longarini, Giovanni P. Rosotti, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Jane Huang, John D. Ilee, Andres F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Teresa Paneque-Carreno, Christophe Pinte, Daniel Price, Jochen Stadler, Richard Teague, Sierk van Terwisga, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki, Ke Zhang
Figure caption: Histogram of the median peak CO abundances, split between the Herbig disks (in red) and the T Tauri disks (in blue).
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: LCO 2.0 m/MuSCAT3 light curves of the target, BD+05 4868 A, and its fainter binary companion, BD+05 4868 B, obtained on UT 2024 October 17. (a) The light curves of each of the four bands are shown in the top panels, with the data in small gray points overplotted by binned light curves. The gp, rp, ip, and zs binned light curves are plotted in blue circles, green triangles, orange squares, and red diamonds, respectively. The BD+05 4868 A light curve is also shown in the bottom panel, indicating that it is similar in depth and overall shape to that of the TESS light curves (red solid line), although there is a small difference due the varying shape of the transits across each orbit (see Figure 8). (e) A comparison of transits in the LCO light curve with the observed mean transit profile from TESS data. A small flux offset was applied to the LCO light curves in this panel to align them with the TESS transit profile.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: TESS light curve of BD+05 4868 A. (a) Normalized and detrended light curves from Sectors 55 and 82. (b) Phase-folded light curve, repeated for two periods. The light curve is folded at a period of 1.271869 days (∼30.5 hr) and binned over 6 minute intervals (red), showing the average transit profile across 29 transits. (c) Close-up of the transit in the phase-folded light curve.
Paper: Biases from Missing a Small Planet in High Multiplicity Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Matthias Y. He
Figure caption: Cumulative distribution functions of gap complexity (top), mass partitioning (bottom left), and impact parameter dispersion (bottom right) for 100 combined SysSim synthetic planet catalogs. The solid lines (dark red) represent the underlying systems, while the dotted lines (red) represent the detected sample. In the top right panel, the detected sample is split between systems with all undetected planets being edge planets (red) and systems with at least one middle planet undetected (orange). In the bottom right panel, there is a third distribution (orange) that shows the impact parameter dispersion of only the transiting planets from the underlying catalog.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: A zoomed-in view of the target, BD+05 4868 A, and its fainter binary companion, BD+05 4868 B, located 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩0 to the northeast. This image is taken from one of the rp-band frames obtained with the LCOGT 2.0 m/MuSCAT3 on the night of UT 2024 October 17. It shows that the two binary components were resolved in this observation. Figure 4 shows the light curves extracted from the MuSCAT3 data obtained that night.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Spectral energy distribution (SED) of BD+05 4868 AB. The crosses show the observed broadband photometry, with horizontal widths indicating the filter bandwidths. The circles represent the model fluxes in the corresponding bands. Colors denote whether the observation corresponds to the primary star (green), secondary star (yellow), or the blended pair (blue). The bottom panel shows the deviations between the data and the model divided by the photometric uncertainties. For illustrative purposes, we also show the R. L. Kurucz (1993) model atmospheres for the best-fitting stellar models. These models were not used directly in the fit, although they were used to generate the MIST bolometric correction tables.
Paper: Biases from Missing a Small Planet in High Multiplicity Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Matthias Y. He
Figure caption: Comparing the cumulative distribution functions of gap complexity (top), mass partitioning (bottom left), and impact parameter dispersion (bottom right) for 80 4+ planet L24 systems (dark blue, solid) to 100 combined SysSim synthetic planet catalogs (red, dotted). In the top right panel, the detected sample is split between systems with all undetected planets being edge planets (red) and systems with at least one middle planet undetected (orange).
Paper: First JWST/NIRSpec Spectroscopy of O Stars in the Small Magellanic Cloud
Authors: Armin Mang Román, Peter Zeidler, Wolf-Rainer Hamann, Lidia M. Oskinova, M. J. Rickard, S. Reyero Serantes, H. Todt, J. S. Gallagher, D. Massa, D. Pauli, V. Ramachandran, E. Sabbi, A. A. C. Sander
Figure caption: Comparison of observations and the stellar atmosphere model computed with parameters derived by M. J. Rickard et al. (2022) for the O8V star SSN 18. Top panel: synthetic SED (red line) adjusted to the HST/STIS UV spectrum, HST/ACS photometry in the F555W (14.470  ±  0.003 mag) and F814W (14.672  ±  0.004 mag) filters, JWST/NIRCam photometry in the F444W (18.786  ±  0.002 mag) filter, and the JWST/NIRSpec spectrum (blue lines and boxes). The red-hatched boxes are centered on synthetic magnitudes derived from the model spectrum. The size of the photometry boxes does not represent uncertainties. The luminosity and reddening indicated in the insert are revised down to match the infrared observations. The black dashed line is the synthetic SED computed with the previous reddening and luminosity values. Bottom panels: observed line profiles of C IV λλ 1548.2, 1550.8 Å, Hα, and Brα, located in the UV, optical, and IR spectra (blue solid lines) compared with models with ﹩{\mathrm{log}}\,\dot{M}=-8.45﹩ (red solid line), ﹩{\mathrm{log}}\,\dot{M}=-8.4\,﹩ (black dashed line), and ﹩{\mathrm{log}}\,\dot{M}=-9.1﹩ (green dotted–dashed line). The excess absorption in the observed Hα profile is most likely an artifact by an oversubtraction of nebular emission.
Paper: ASKAP and VLASS Search for a Radio-continuum Counterpart of Ultra-high-energy Neutrino Event KM3–230213A
Authors: M. D. Filipović, Z. J. Smeaton, A. C. Bradley, D. Dobie, B. S. Koribalski, R. Kothes, L. Rudnick, A. Ahmad, R. Z. E. Alsaberi, C. S. Anderson, L. A. Barnes, M. Breuhaus, E. J. Crawford, S. Dai, Y. A. Gordon, N. Gupta, A. M. Hopkins, D. Leahy, K. J. Luken, N. McClure-Griffiths, M. J. Michałowski, M. Sasaki, N. F. H. Tothill, G. M. Umana, T. Vernstrom, J. West
Figure caption: Multifrequency and spectral index maps of the galaxy UGCA 127 (Phaedra). Top left: MeerKAT 1.3 GHz radio-continuum image. The radio components to the east and west of the galaxy core and the X-ray source 2SXPS J062057.7–082939 are annotated. The synthesized beam (7﹩\mathop{.}\limits^{^{\prime\prime} }﹩68 × 7﹩\mathop{.}\limits^{^{\prime\prime} }﹩52, P.A. = –40°) is shown in the bottom left corner. The image has a local rms noise level of  ∼15 μJy beam−1. Top right: ASKAP 944 MHz radio-continuum image. The 15″ synthesized beam is shown in the bottom left corner. The image has a local rms noise level of  ∼50 μJy beam−1. Bottom left: spectral index map zoomed to show only the central emission. The map was generated using the high-resolution ASKAP 944 MHz image, the MeerKAT 1.3 GHz image, and the 3-epoch-averaged VLASS 3 GHz image as described in Section 2.2.2. The final image was convolved to 10″. Bottom right: multifrequency RGB image, consisting of MeerKAT 1.3 GHz (red), optical DSS2 R-band (green), and WISE 3.4 μm (blue) images. All images are linearly scaled, and the bottom row includes MeerKAT 1.3 GHz radio contours at levels of 10, 20, 30, 50, 100, and 150 σ, where 1 σ = 15 μJy beam−1.
Paper: First JWST/NIRSpec Spectroscopy of O Stars in the Small Magellanic Cloud
Authors: Armin Mang Román, Peter Zeidler, Wolf-Rainer Hamann, Lidia M. Oskinova, M. J. Rickard, S. Reyero Serantes, H. Todt, J. S. Gallagher, D. Massa, D. Pauli, V. Ramachandran, E. Sabbi, A. A. C. Sander
Figure caption: NIRCam image of NGC 346 with lines connecting the NIRSpec spectrum to the position of each star of our sample. Catalog names (SSN) come from E. Sabbi et al. (2007), while the spectral types are adopted from M. J. Rickard et al. (2022). The image is a color composite of the F277W (blue), F335M (green), and F400W (red) filters. The broadband filters show the stellar and galaxy continuum emission, while F335M highlights the polycyclic aromatic hydrocarbon (PAH) emission at 3.3 m. North is up, and east is left. The image covers an area on the sky of ﹩5.\,^{\prime} 4\,\times 6.\,^{\prime} \,7﹩ that is equal to ∼96 pc × 119 pc at a distance of 61 kpc. The calibrated spectra cover a wavelength range between 2.8 and 5.1 μm range, and the fluxes are between −18 and −16 in log fλ /[ers s−1 cm−1 s−1 Å].
Paper: ASKAP and VLASS Search for a Radio-continuum Counterpart of Ultra-high-energy Neutrino Event KM3–230213A
Authors: M. D. Filipović, Z. J. Smeaton, A. C. Bradley, D. Dobie, B. S. Koribalski, R. Kothes, L. Rudnick, A. Ahmad, R. Z. E. Alsaberi, C. S. Anderson, L. A. Barnes, M. Breuhaus, E. J. Crawford, S. Dai, Y. A. Gordon, N. Gupta, A. M. Hopkins, D. Leahy, K. J. Luken, N. McClure-Griffiths, M. J. Michałowski, M. Sasaki, N. F. H. Tothill, G. M. Umana, T. Vernstrom, J. West
Figure caption: ASKAP 944 MHz radio-continuum image, SB 59692. The cyan-colored circle (radius = 1﹩\mathop{.}\limits^{^\circ }﹩5) indicates the 68% confidence area of the neutrino event. The image is linearly scaled and has a synthesized beam of 15″. Colored squares show the locations of three objects of interest: the white square shows the variable source Narcissus (EMU J062244–072333; see Section 2.2.4), the yellow square shows Hebe (WISEA J061715.89–075455.4; see Section 2.2.3), and the blue square shows Phaedra (UGCA 127; see Section 2.2.2).
Paper: First JWST/NIRSpec Spectroscopy of O Stars in the Small Magellanic Cloud
Authors: Armin Mang Román, Peter Zeidler, Wolf-Rainer Hamann, Lidia M. Oskinova, M. J. Rickard, S. Reyero Serantes, H. Todt, J. S. Gallagher, D. Massa, D. Pauli, V. Ramachandran, E. Sabbi, A. A. C. Sander
Figure caption: Zoom-in (3﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 × 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩1) of the F187N NIRCam image for two targets that required manual treatment on the background subtraction. The yellow shaded area indicates the position of the slit in the different dithers, with the darker area being the overlap. North is up, and east is left. SSN 14 (left panel) is located in a very crowded field, with multiple objects falling into the slit (yellow dots indicate JWST/NIRCam catalog sources). SSN 43 (right panel) is the faintest target of the sample and is highly susceptible to spatial background variations.
Paper: First JWST/NIRSpec Spectroscopy of O Stars in the Small Magellanic Cloud
Authors: Armin Mang Román, Peter Zeidler, Wolf-Rainer Hamann, Lidia M. Oskinova, M. J. Rickard, S. Reyero Serantes, H. Todt, J. S. Gallagher, D. Massa, D. Pauli, V. Ramachandran, E. Sabbi, A. A. C. Sander
Figure caption: Comparison between the background-subtracted spectra around Brα with the default nod-subtraction (solid black line) and manual subtraction (dashed blue line) for two different targets, SSN 14 (top panel) and SSN 43 (bottom panel). The vertical gray line marks the position of the Brα emission peak in the nonsubtracted background. In both cases, the default method oversubtracts the background, while the manual method results in a more reliable line profile.
Paper: First JWST/NIRSpec Spectroscopy of O Stars in the Small Magellanic Cloud
Authors: Armin Mang Román, Peter Zeidler, Wolf-Rainer Hamann, Lidia M. Oskinova, M. J. Rickard, S. Reyero Serantes, H. Todt, J. S. Gallagher, D. Massa, D. Pauli, V. Ramachandran, E. Sabbi, A. A. C. Sander
Figure caption: Observed Brα line profiles for 12 targets of our sample.
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): A Unified Evolutionary Sequence of Planet-driven Substructures Explaining the Diversity of Disk Morphologies
Authors: Santiago Orcajo, Lucas A. Cieza, Octavio Guilera, Sebastián Pérez, Fernando R. Rannou, Camilo González-Ruilova, Grace Batalla-Falcon, Trisha Bhowmik, Prachi Chavan, Simon Casassus, Anuroop Dasgupta, Kevin Diaz, José L. Gomez, Antonio S. Hales, J. M. Miley, Marcelo M. Miller Bertolami, P.H. Nogueira, María Paula Ronco, Dary Ruiz-Rodriguez, Anibal Sierra, Julia Venturini, Philipp Weber, Jonathan P. Williams, Alice Zurlo
Figure caption: The top panels show our models, the same as in Figure 4, illustrating each of the five stages. The rest of the panels contain the 15 brightest disks in Ophiuchus studied by C21 in the stage (column) in which they have been classified. The figure illustrates the key characteristic features of each stage and also the observed diversity (see Section 4.3 for discussion).
Paper: ASKAP and VLASS Search for a Radio-continuum Counterpart of Ultra-high-energy Neutrino Event KM3–230213A
Authors: M. D. Filipović, Z. J. Smeaton, A. C. Bradley, D. Dobie, B. S. Koribalski, R. Kothes, L. Rudnick, A. Ahmad, R. Z. E. Alsaberi, C. S. Anderson, L. A. Barnes, M. Breuhaus, E. J. Crawford, S. Dai, Y. A. Gordon, N. Gupta, A. M. Hopkins, D. Leahy, K. J. Luken, N. McClure-Griffiths, M. J. Michałowski, M. Sasaki, N. F. H. Tothill, G. M. Umana, T. Vernstrom, J. West
Figure caption: Left: broadband spectrum of Narcissus (EMU J062244–072333, including minor contributions from EMU J062248–072246 low frequencies, from the larger beams). Values from all three VLASS epochs are shown. The illustrative spectra are for a homogeneous self-absorbed synchrotron source, with an optical depth of 1 at 600 MHz and an optically thin index of –0.5 (pink), and synchrotron emission from a subrelativistic shock of thermal electrons at frequencies below the thermal cooling threshold, with an optically thin slope of –0.15 (blue). Middle: overlay of the two radio sources from the VLASS map averaged over all epochs on the WISE W1 image. Right: overlay on the multiband PanSTARRS image.
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): A Unified Evolutionary Sequence of Planet-driven Substructures Explaining the Diversity of Disk Morphologies
Authors: Santiago Orcajo, Lucas A. Cieza, Octavio Guilera, Sebastián Pérez, Fernando R. Rannou, Camilo González-Ruilova, Grace Batalla-Falcon, Trisha Bhowmik, Prachi Chavan, Simon Casassus, Anuroop Dasgupta, Kevin Diaz, José L. Gomez, Antonio S. Hales, J. M. Miley, Marcelo M. Miller Bertolami, P.H. Nogueira, María Paula Ronco, Dary Ruiz-Rodriguez, Anibal Sierra, Julia Venturini, Philipp Weber, Jonathan P. Williams, Alice Zurlo
Figure caption: Top panels: models with 1 MJup planet. The left panel shows the surface density profiles of our fiducial model. The dashed green line corresponds to the initial gas surface density, while the solid lines indicate the evolution of the dust surface density in steps of 25,000 yr after a 1 MJup planet has been injected at 57 au. The right panel shows the maximum grain size as a function of radius of the fiducial model after 0.1 Myr evolution. The color scale corresponds to the integrated surface density at the given radius. As expected, the dust accumulates and grows at the outer edge of the gap. Bottom panels: same as the top panels but for the model with a Mars-mass planet, which we use to represent stage I. While no gap is produced, an inflection point in the surface density profile and the grain size distribution is seen close to the location of the planet.
Paper: ASKAP and VLASS Search for a Radio-continuum Counterpart of Ultra-high-energy Neutrino Event KM3–230213A
Authors: M. D. Filipović, Z. J. Smeaton, A. C. Bradley, D. Dobie, B. S. Koribalski, R. Kothes, L. Rudnick, A. Ahmad, R. Z. E. Alsaberi, C. S. Anderson, L. A. Barnes, M. Breuhaus, E. J. Crawford, S. Dai, Y. A. Gordon, N. Gupta, A. M. Hopkins, D. Leahy, K. J. Luken, N. McClure-Griffiths, M. J. Michałowski, M. Sasaki, N. F. H. Tothill, G. M. Umana, T. Vernstrom, J. West
Figure caption: Left: polarized intensity of Hebe at 944 MHz, overlaid with white contours of total intensity at (0.5, 1, 1.5, 2, 4,...) mJy beam−1. The cyan line indicates the orientation of the inferred magnetic field at the polarized peak after Faraday rotation correction, and the magenta contours are of the WISE W1 image. Right: PanSTARRS image, combining the z, i, and r frames, overlaid with contours of polarized intensity at 0.5, 0.8, and 0.9 mJy beam−1. The faint optical envelope is seen, in more burned-out images, to encompass all three galaxies.
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): A Unified Evolutionary Sequence of Planet-driven Substructures Explaining the Diversity of Disk Morphologies
Authors: Santiago Orcajo, Lucas A. Cieza, Octavio Guilera, Sebastián Pérez, Fernando R. Rannou, Camilo González-Ruilova, Grace Batalla-Falcon, Trisha Bhowmik, Prachi Chavan, Simon Casassus, Anuroop Dasgupta, Kevin Diaz, José L. Gomez, Antonio S. Hales, J. M. Miley, Marcelo M. Miller Bertolami, P.H. Nogueira, María Paula Ronco, Dary Ruiz-Rodriguez, Anibal Sierra, Julia Venturini, Philipp Weber, Jonathan P. Williams, Alice Zurlo
Figure caption: From the top to bottom, variation of Mp, α, dust-to-gas mass ratio, and Mdisk/Mstar, compared with the fiducial model (blue mark).
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): A Unified Evolutionary Sequence of Planet-driven Substructures Explaining the Diversity of Disk Morphologies
Authors: Santiago Orcajo, Lucas A. Cieza, Octavio Guilera, Sebastián Pérez, Fernando R. Rannou, Camilo González-Ruilova, Grace Batalla-Falcon, Trisha Bhowmik, Prachi Chavan, Simon Casassus, Anuroop Dasgupta, Kevin Diaz, José L. Gomez, Antonio S. Hales, J. M. Miley, Marcelo M. Miller Bertolami, P.H. Nogueira, María Paula Ronco, Dary Ruiz-Rodriguez, Anibal Sierra, Julia Venturini, Philipp Weber, Jonathan P. Williams, Alice Zurlo
Figure caption: The temporal evolution for fiducial models with the 1 MJup planet, from 20 kyr to 2.5 Myr. The top five panels show steps of 20 kyr, the middle panels correspond to steps of 100 kyr, and the bottom panels illustrate steps of 500 kyr. Each panel corresponds to the synthetic image at 1.3 mm of the PLANETALP model, produced via radiative transfer and ray tracing with RADMC-3D.
Paper: ASKAP and VLASS Search for a Radio-continuum Counterpart of Ultra-high-energy Neutrino Event KM3–230213A
Authors: M. D. Filipović, Z. J. Smeaton, A. C. Bradley, D. Dobie, B. S. Koribalski, R. Kothes, L. Rudnick, A. Ahmad, R. Z. E. Alsaberi, C. S. Anderson, L. A. Barnes, M. Breuhaus, E. J. Crawford, S. Dai, Y. A. Gordon, N. Gupta, A. M. Hopkins, D. Leahy, K. J. Luken, N. McClure-Griffiths, M. J. Michałowski, M. Sasaki, N. F. H. Tothill, G. M. Umana, T. Vernstrom, J. West
Figure caption: Left: mean H I velocity field of the galaxy UGCA 127 and its companion using data from the H I Parkes All Sky Survey (HIPASS). The Parkes gridded beam (15.5﹩^{\prime} ﹩) is shown in the bottom left corner. Top right: PanSTARRS optical color-composite image using the yig bands. Bottom right: integrated HIPASS spectrum; the 50% and 20% velocity width estimates as well as the peak flux density are indicated.