adsabs/AstroCLIMB huggingface dataset:
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Point-wise fold of 2800 ATLAS archival data points for TIC 290061484. The fold period is 24.498 days, which represents the highest peak in the BLS transform for periods between 10 and 100 days. The eclipses of the inner binary have been removed prior to the BLS transform. Only one of the two outer eclipses appears (near phase 1.0), the other likely being smeared owing to the large jitter inherent in third-body eclipses that depend on both the inner and outer orbital phases. The uncertainty in the mean outer period from the ATLAS data alone is ±0.005 days.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: TESS FITSH light curve of TIC 290061484. Each panel represents a different sector. The deep regular eclipses are from the 1.792-day inner EB. The tertiary eclipses are highlighted with red arrows. Note that the tertiary eclipse near day 2840 is difficult to see on this scale.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption:                       ﹩4^{\prime} \times 4^{\prime} ﹩ PanSTARRS image (K. C. Chambers et al. 2016) centered on TIC 290061492. The small white contour represents one TESS pixel (21″ × 21″) oriented according to Sector 16, and the large white contour represents a ﹩1^{\prime} \times 1^{\prime} ﹩ region. North is up, and east is to the left.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Contrast curves showing the 5σ magnitude limits for the 562 and 832 nm high-resolution speckle observations of TIC 290061484 Left: the reconstructed 832 nm image. Right: close companions can be excluded within 20 mas to 1.″2 of TIC 290061484 at the specified contrast limits.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Panels 1–11, counting from top left: photodynamical model fits highlighting the tertiary eclipses of TIC 290061484 in Sectors 15, 16, 55, 56, 75, and 76. The blue points are the TESS photometric measurements, while the red curve is the model fit. The TESS sector is marked in the lower left corner of each panel. For an easier identification of the shallowest third-body eclipses, all tertiary events are marked with vertical arrows. Note that dashed arrows show two extremely shallow third-body eclipses that are present on the model light curve but cannot be identified in the observations. The middle panel in the last row presents the first tertiary event that has been detected in our ground-based photometric follow-up campaign, at BAO80. Bottom right panel: simulated long-term light curve of TIC 290061484 (red), emphasizing the expected eclipse depth changes. The dense pattern represents the EB eclipses; the thin lines extending below the pattern represent the tertiary eclipses.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Top panel: the variations of the observable and dynamical arguments of periastron of the inner orbit (red and black circles, respectively), as well as the same orbital elements of the outer orbit (blue and gray curves). The vertical, thick gray lines represent the midtimes of the three segments of TESS observations. Bottom panel: the variations of the observable inclinations of both the inner and outer orbits (red and blue curves, respectively). The cyan area represents the domain of the (inner) inclination angle where regular, two-body eclipses may occur, while the two, mostly horizontal, thick black curves represent the borders of the third-body eclipses. As one can see, the inner inclination remains continuously well within its eclipsing domain; hence, the inner EB exhibits permanently deep eclipses. On the other hand, the outer inclination cyclically reaches, and even intersects, the border of the third-body eclipsing domain, which leads to very shallow, grazing, and even disappearing third-body eclipses from time to time.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Top and middle panels: orbital configuration of TIC 290061484 as seen from above the outer orbital plane over the course of 1, 10, 100, and 1000 triple orbits (top left, top right, middle left, and middle right panels, respectively). The individual components are color-coded as indicated in the legend. The observer is in the x-y plane, looking along the y-direction. To highlight the rapid orbital precession of the triple subsystem, the top left, top right, and middle left panels are shown in the center-of-mass reference frame of that system. The middle right panel is shown in the center-of-mass reference frame of the entire quadruple system. Bottom panels: dynamical evolution of the system over the course of 100,000 triple orbits (∼2.5 million days) showing the semimajor axes (left), eccentricity (middle), and inclination (right) for the inner binary (red) and for the outer tertiary (blue). The parameters are plotted once a day for viewing purposes. There are no indications for chaotic motion, and the system is dynamically stable for the duration of the integrations.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Outer vs. inner mass ratios for compact triples with P out < 300 days. We highlight the nine extremely compact triples with P out < 50 days (red plus signs), including TIC 290061484 (red asterisk), and we bracket their two main islands (dotted red lines). A triple where the tertiary is the most massive component lies above the dashed line.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Cumulative SED of the TIC 290061484 system. Red circles represent the (dereddened) catalog passband magnitudes that were used in the SED fitting part of the joint photodynamical analysis. Blue squares stand for the theoretical passband magnitudes interpolated from the PARSEC isochrone grids. For comparison we plotted the theoretical ATLAS model atmosphere SEDs (F. Castelli & R. L. Kurucz 2003) for the entire system (thick black line representing the cumulative SED) and for the individual stars (thin red line: star B; thin blue line: star Aa; thin green line: stars Ab and C).
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: MIST radius evolution vs. time for the four stars in the TIC 290061484 system (the MIST tracks are from B. Paxton et al. 2011, 2013, 2015; A. Dotter 2016; J. Choi et al. 2016; and B. Paxton et al. 2018). The system is currently ∼14 Myr old (marked with an arrow). The most massive star, B, will ascend the giant branch at ∼36 Myr and begin to transfer mass to the inner binary (blue circle) shortly before star Aa fills its Roche lobe in the inner binary (∼45 Myr; green circle). What may happen during both of the mass transfer events is described in Section 6.8.
Paper: TIC 290061484: A Triply Eclipsing Triple System with the Shortest Known Outer Period of 24.5 Days
Authors: V. B. Kostov, S. A. Rappaport, T. Borkovits, B. P. Powell, R. Gagliano, M. Omohundro, I. B. Bíró, M. Moe, S. B. Howell, T. Mitnyan, C. A. Clark, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, A. Pál, A. Vanderburg
Figure caption: Cumulative distributions of tertiary periods P out for the simulated population (black) and 59 observed compact triples with P out < 300 days (red).
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: A schematic illustration of the present-day LMC with respect to the MW disk. The locations, orientations, and sizes of the LMC (star-forming) disk and a potential bow shock are based on a hydrodynamic simulation of the LMC orbiting in the MW halo (Setton et al. 2023, see their Figure 4); the simulation assumes the LMC to be on its first infall (Besla et al. 2007). The location of the Small Magellanic Cloud (SMC) is indicated as a cross. We highlight in blue arrows the LMC’s outflows on its nearside, which we study in this work using 110 sight lines from the ULLYSES DR5. We also show the location of a foreground high-velocity cloud at d ⊙ < 13.3 kpc (Richter et al. 2015; Werner & Rauch 2015), which contaminates potential LMC outflow absorption over v helio ∼ 90–175 km s−1. Our work focuses on the LMC gas at v helio = 175–375 km s−1 to minimize foreground contamination.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Velocity offsets between the multiphase gas (H I, S II, Si IV, and C IV) and the LMC’s young stellar disk, δ v bulk (Equation (5)), as a function of ΣSFR. The bars on the right sides show histogram distributions of δ v bulk. The top left panel shows that the H I gas largely follows the rotation of the LMC’s young stellar disk. For S II, Si IV, and C IV, negative offset velocities indicate outflows; we refer to the negative values at δ v bulk < −15 km s−1 as outflow velocities and discuss them in absolute values ∣v out, bulk∣. We conservatively do not consider data points within ∣δ v bulk∣ < 15 km s−1 (gray bands) to avoid the LMC’s ISM. Generally, we find outflows in S II, Si IV, and C IV with bulk velocities of ∣v out, bulk∣ ∼ 20–60 km s−1, suggesting that the bulk mass of the outflowing gas should be gravitationally bound. At the higher ΣSFR end, we only detect outflows in Si IV and C IV but not in S II, suggesting that star-forming regions with higher ΣSFR are likely to launch outflows that are more ionized. See Section 4.2 for further details.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Top: gas column density as a function of ΣSFR in logarithmic values for H I, S II, Si IV, and C IV, respectively. Solid circles are detections, open squares with upward arrows are saturations with lower limits (only in S II, Si IV, and C IV), and open triangles with downward arrows are nondetections (only in H I). The error bars on the x-axis (∼0.02–0.06 dex) are smaller than the symbol sizes. Bottom: 2D spatial distributions of H I, S II, Si IV, and C IV column densities in the same orthographic projection as shown in Figure 3. For S II, Si IV, and C IV, the shown ﹩\mathrm{log}N﹩ values/colors in bins noted with upward arrows should be considered as conservative lower limits. Several major H ii regions are highlighted as crosses in each panel. We find high ion column densities correlate with regions with high star-forming activities, such as 30 Dor at x ∼ 1.°5 and y ∼ 0°. See Section 4.1 for further details.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Distribution of the ULLYSES sight lines against the Hα map in an orthographic projection in the LMC plane, following the method outlined in Choi et al. (2022). At the distance of the LMC (50.1 kpc) (Freedman et al. 2001), 1 deg ≈0.9 kpc. Major H II regions are indicated by blue crosses. Gray-filled circles indicate those sight lines with reliable S II (91/110; left), Si IV (44/110; middle), and C IV (71/109; right) measurements over the LMC’s absorption range of v helio = 175–375 km s−1. An ion measurement is considered reliable if (1) its stellar continuum shows a strong P Cygni profile such that the LMC’s interstellar absorption can be reliably identified, and (2) the column density difference between doublet lines is within what is allowed by the apparent optical depth method (Savage & Sembach 1991, 1996). See Section 2 for further details.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Normalized S II, Si IV, and C IV spectra for SK-67D104 (left) and SK-71D41 (right). We highlight three velocity components: (1) the MW’s ISM and intermediate velocity cloud at v ≲ 90 km s−1 (gray), (2) a high-velocity cloud at 90 ≲ v ≲ 175 km s−1 and d ⊙ < 13.3 kpc in the foreground (HVC90-175 (orange)), and (3) the LMC’s ISM and outflows at 175 ≲ v ≲ 375 km s−1 (blue). The relative spatial locations of the three components are sketched in Figure 1. The solid vertical lines show the velocities of the LMC’s stellar disk at the locations of the stars (see Section 3). The left panel shows an example sight line where the absorption from HVC90-175 and the LMC (ISM+outflows) can be well separated near v = 175 km s−1, while the right panel shows an example where the two components are blended. We quantify the degree of blending between HVC90-175 and the LMC absorption near v = 175 km s−1 in Section 2.4.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Left: example spectra with well-developed P Cygni profiles in Si IV (see Section 2.3), with fluxes in black curves and errors in gray. The MW and LMC Si IV absorption can be reliably separated from the stellar P Cygni profiles. We show in red curves the best-fit continuum models, which we discuss in Section 2.4. Right: example spectra that have either mild or no stellar winds, in which case the Si IV absorption from stellar photospheres blends heavily with the MW and LMC interstellar absorption; we consider these Si IV unreliable. In each panel, the blue and red vertical shades indicate the stellar continuum regions that we use to calculate the wind ratios f  w  (Equation (1)) to quantify the strengths of stellar winds/P Cygni profiles.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: 2D distribution of δ v bulk (Equation (5)) for S II (left), Si IV (middle), and C IV (right) in the same orthographic projection as in Figure 3 and in units of kilometers per second. Gray indicates regions with ionized gas kinematics consistent with the LMC’s stellar disk (and ISM) within ±15 km s−1, blue for bulk outflows, and red for bulk inflows. Major H II regions are indicated by crosses. We find disk-wide ionized outflows in S II, Si IV and C IV with bulk velocities of ∣v out, bulk∣ ∼ 20–60 km s−1. See Section 4.2 for further details.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Distribution of 110 ULLYSES DR5 stellar sight lines (black circles) across the LMC. The left panel shows an H I column density map (Kim et al. 2003) and the right panel shows a continuum-subtracted Hα intensity map of the LMC (Gaustad et al. 2001). Red and blue crosses in the left and right panels indicate several major H II regions in the LMC, respectively. We introduce the ULLYSES data set in Section 2, and the H I and Hα data sets in Section 3.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Distribution of stars with reliable C IV (top), Si IV (middle), and S II (bottom panel) LMC interstellar absorption as a function of spectral type. Those sight lines that we adopt in our LMC analysis (i.e., reliable) are shown in blue, red, and orange, respectively, and those that we consider unreliable and thus discarded are shown in gray. See discussion in Section 2.5.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Histogram distributions of the ULLYSES DR5 sight lines as a function of ΣSFR in logarithmic values. Sight lines with reliable C IV (top), Si IV (middle), and S II (bottom) are highlighted in blue, orange, and red, respectively.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: A scaling relation between bulk outflow velocity and ΣSFR in logarithmic values. We compare the LMC outflows (red-filled circles) with three studies, including H15, (green-filled triangles), C15 (yellow-filled squares), and ​​​​​​X22 (magenta-filled diamonds), on cool outflows in starburst galaxies that used the same or similar instruments (either HST or FUSE) to minimize systemic uncertainties. The solid black line shows our best-fit power-law relation, ﹩\mathrm{log}{v}_{\mathrm{out},\ \mathrm{bulk}}=0.23\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{SFR}}+1.98﹩ or ﹩{v}_{\mathrm{out},\ \mathrm{bulk}}=\,95.5\,\mathrm{km}\,{{\rm{s}}}^{-1}\,{{\rm{\Sigma }}}_{\mathrm{SFR}}^{0.23}﹩, for the observational data points, where the dark and light blue shades indicate the 68% and 95% confidence intervals. Gray-filled circles show simulation predictions from the TIGRESS-classic simulation suite over a wide range of star-forming conditions (Kim et al. 2020). The best-fit scaling relation from Kim et al. (2020) is shown as a black dashed line. See Section 5 for further details.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: 2D distributions of H I, S II, Si IV, and C IV bulk velocities in the heliocentric frame and in units of kilometers per second. The systemic velocity of the LMC at the center of its mass (x, y) = (0°, 0°) is v sys = 264 km s−1 (Choi et al. 2022), which is shown as a gray color. Major H II regions are indicated by black crosses. All ions show signs of corotation with the LMC’s disk. See Section 4.3 for further details.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: Multiphase ion velocities of HVC90-175 as a function of R.A. in the LSR (left), GSR (middle), and LMCSR (right) frames (see Equation (A1)). HVC90-175 is detected in low ions such as O I (yellow-filled circles; Lehner et al. 2009, see also Roman-Duval et al. 2019) as well as in S II, Si IV, and C IV (this work). HVC90-175's gas kinematics is consistent with being an MW halo cloud at v LSR = 120 km s−1 with a temperature of T = 104.2 K and a nonthermal broadening of σ nth ∼ 10 km s−1. The distance to HVC90-175 is constrained to be d ⊙ < 13.3 kpc (Richter et al. 2015; Werner & Rauch 2015).