adsabs/AstroCLIMB huggingface dataset:
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: 4–8 GHz BL GC survey footprint covered by 19 spatial pointings (colored circles), each of HPBW ﹩\approx 2\buildrel{\,\prime}\over{.} 5﹩. Various colors indicate pointings that have been grouped together for position-switched observations.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: Narrowband CW transmitter rate vs. minimum detectable EIRP for different surveys (various markers). Markers containing a white dot in their interior label surveys targeting exoplanets known to reside in the habitable zones around their host stars. The solid gray vertical line marks EIRP ≃ 1013 W of an Arecibo-like transmitter. The dashed gray vertical line represents the the total solar power incident on the Earth. The diagonal gray band is a power-law fit derived from the best constraining limits (Gray & Mooley 2017; Price et al. 2020) on the CW transmitter rate at the low and high EIRP ends. Assuming a power-law distribution (N et ∝ EIRP α ) of transmitters in our galaxy, the slope α ≈ −0.66 of our power-law fit constrains the luminosity function of extraterrestrial CW transmitters between EIRP limits of 2 × 1012 W to 2 × 1021 W. Plotted points for past surveys are taken from Figure 13 of Gajjar et al. (2021).
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: Our true search sensitivity ﹩{\mathrm{EIRP}}_{\mathrm{true}}^{\min }﹩ in the P-δ plane measured via injection of fake periodic signals into GBT time-series data. The color scale quantifies ﹩{\mathrm{EIRP}}_{\mathrm{true}}^{\min }﹩ relative to the theoretical sensitivity ﹩{\mathrm{EIRP}}_{\mathrm{periodic}}^{\min }﹩ estimated from Equation (6). Black circular markers label trial (P, δ) of fake signal injections.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: Occurrence rate of 4–8 GHz extraterrestrial transmitters of kHz-wide periodic pulsed signals measured as a function of EIRP for a pulse duty cycle, δ ≃ 10%. The hatched region represents the parameter space excluded by our nondetection of channel-wide periodic signals in the 4–8 GHz BL GC survey.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Comparison of differences in average H I line profile parameters as measured by us with averages of values listed in the literature, for the galaxies in our combined sample. Plotted as a function of our average H I line parameters are the differences in: (a) central velocity, ΔV H I  in kilometers per second, (b) ΔW 50 line width, in kilometers per second, and (c) integrated line flux, ΔF H I in Jansky kilometers per second. As indicated in the legend, colors indicate the probability of a detection being confused by another galaxy within the telescope beam: black for uncontaminated, blue for possibly contaminated, and red for likely contaminated. Please note that panel (a) does not include PGC 38958 (see the Appendix for an explanation).
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Comparison of the cumulative distributions of our two galaxy samples (HyperLeda in black, UGC in red) and the HIPASS BGC (blue) with (a) total H I mass, log(M H I ) in solar masses, and (b) total dynamical mass, as represented by the measured W 50 H I line width, uncorrected for inclination. The blue vertical line in (a) shows the massive LSB galaxy limit.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Plotted as a function of mean blue surface brightness, 〈μ B〉 in magnitude per arcsecond2, are (a) the total H I mass, log(M H I  ) in solar masses, and (b) the inclination-corrected W 50,cor H I line width in kilometers per second, for the detected galaxies in our combined sample. As indicated in the legend, colors indicate the probability of a detection being confused by another galaxy within the telescope beam: black for uncontaminated, blue for possibly contaminated, and red for likely contaminated.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Plotted as a function of mean blue surface brightness, 〈μ B〉 (in magnitude per arcsecond2), are (a) the blue luminosity, log(L B) in L ⊙,B and (b) the log(M H I /L B) H I mass-to-light ratio ratio, in solar units, for the galaxies in our combined sample. As indicated in the legend, colors indicate the probability of a detection being confused by another galaxy within the telescope beam: black for uncontaminated, blue for possibly contaminated, and red for likely contaminated.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Differences between our central H I line velocities and averaged values of the optical velocities listed in the literature, ΔV opt in kilometers per second, as a function of optical velocities from the literature, V hel kilometers per second, for the galaxies in our combined sample. As indicated in the legend, colors indicate the probability of a detection being confused by another galaxy within the telescope beam: black for uncontaminated, blue for possibly contaminated, and red for likely contaminated.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Total H I mass, log(M H I ) in solar masses, as a function of total mass, as represented by the inclination-corrected W 50,cor H I line velocity width (in kilometers per second) for the detected galaxies in our combined sample. As indicated in the legend, colors indicate the probability of a detection being confused by another galaxy within the telescope beam: black for uncontaminated, blue for possibly contaminated, and red for likely contaminated.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Total H I mass, log(M H I ) in solar masses, as a function of radial velocity, V hel in kilometers per second, for the detected galaxies in our combined sample. As indicated in the legend, symbols indicate the probability of a detection being confused by another galaxy within the telescope beam: solid for uncontaminated, open for possibly contaminated, and small for likely contaminated.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: DSS multicolor (IR, red, and blue plates) image of PGC 3843 (center, white cross). The large white circle shows the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam, and the cyan circles denote the two galaxies which have likely recently interacted with PGC 3843, WISEA J010444.68-110422.9 and MCG-02-03-071. The image is 25′ across.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Optical images of ESO 491-002. A B-band image (left) from Lauberts & Valentijn (1989) taken at the ESO 1 m Schmidt telescope shows an LSB object, which could be a distorted galaxy, but no galaxy is discernible on the DSS2 B, R, or IR images (Abazajian et al. 2004) taken with the 1.2 m Palomar Schmidt telescope. Images are ﹩4\buildrel{\,\prime}\over{.} 3﹩ × ﹩4\buildrel{\,\prime}\over{.} 3﹩ in size.
Paper: Magnetic Effects and 3D Structure in Theoretical High-resolution Transmission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Arjun B. Savel
Figure caption: Simulated high-resolution transmission spectra from our 3 G model, with Doppler effects from winds and rotation, shown at equally spaced times throughout transit. As expected, midtransit (phase = 0) has the strongest absorption since the maximum amount of light is obscured by the planet’s atmosphere at this phase. The first and last phases shown here are partial transits, which is why their continuum values are lower compared to the other spectra shown. We can compare spectra that are equally spaced in time before and after midtransit to identify differences due to east–west asymmetries around the terminator. While the phases nearest to midtransit are very similar, those phases further away show larger differences, with the spectra near the end of transit (where only a portion of the planet is transiting the host star) showing very sharply blueshifted lines.
Paper: Magnetic Effects and 3D Structure in Theoretical High-resolution Transmission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Arjun B. Savel
Figure caption: Net Doppler shifts for the simulated spectra from each model, over the three wavelength regimes considered, as well as the data from Ehrenreich et al. (2020). Overall, the net behavior shows the spectra becoming more blueshifted as transit proceeds. However, the 3 G active drag model shows some deviations from this shortly after midtransit, but only when water is the dominant absorber within the wavelength range considered. When iron is the dominant absorber, we see instead that the starting net redshift persists longer into transit, before switching to a net blueshift. Both of these behaviors are unique to the 3 G model, distinguishing it from the 0 G or Uniform drag models.
Paper: Magnetic Effects and 3D Structure in Theoretical High-resolution Transmission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Arjun B. Savel
Figure caption: Cross-correlation curves for each model throughout transit (with the first and last points being partial ingress and egress respectively) for wavelength range 1 (1.135–1.355 μm). The peak of the cross-correlation curve, corresponding to the net Doppler shift of the spectrum are shown with colored points. These net Doppler shifts vary with time and differ between models due to the differing circulation patterns. Notably, for this wavelength range, the 3 G spectrum become less blueshifted for a time near the end of transit. This is a unique feature of the 3 G model and is a result of the differing wind structure caused by the active magnetic drag prescription.
Paper: Magnetic Effects and 3D Structure in Theoretical High-resolution Transmission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Arjun B. Savel
Figure caption: Temperature projections for the three models used in this analysis, for pressures less than ∼0.1 bars. Note that the core and atmosphere are not to scale, but the relative altitudes at different locations are accurately plotted. The east and west limb asymmetries in spatial extent is a result of the difference in scale heights of each region due to nonuniform temperatures between the east and west terminators. Because of the planet’s short orbital period, it rotates considerably (>30°) between ingress to egress, which is reflected above.
Paper: Magnetic Effects and 3D Structure in Theoretical High-resolution Transmission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Arjun B. Savel
Figure caption: Line-of-sight velocities for the three models considered in this work at ingress, midtransit, and egress. Throughout transit, the blueshifts dominate the net Doppler shift for all models, though the magnitudes of the net Doppler shifts are both model and wavelength dependent.
Paper: Magnetic Effects and 3D Structure in Theoretical High-resolution Transmission Spectra of Ultrahot Jupiters: the Case of WASP-76b
Authors: Hayley Beltz, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Arjun B. Savel
Figure caption: Midtransit (phase = 0) spectra from our three models. The solid lines show spectra that have been shaped by Doppler shifts due to winds and rotation while the dotted curves do not have this influence. Vertical offsets have been added for clarity. Differences between the spectral features are due to the different temperature and wind patterns of the models. All three models have similar vertical temperature structures, and so the spectra without Doppler effects are only very subtly different, while the different wind patterns between the models result in noticeable differences in the resulting spectra.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: SDSS DR12 false color (i, r, and g filters) image of the galaxies with known redshifts lying within the GBT beam centered on PGC 21907 (cyan circle). The large white circle shows the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam. The blue circle denotes the nearest galaxy, SDSS J074933.51+394424.3, the two cyan circles denote galaxies KUG 0746+398A (left) and SDSS J074939.55+394316.7 (right), the green circle PGC 21907 (aka KUG 0746+398B), and the red circles denote the three Wide-field Infrared Survey Explorer (WISE) galaxies which lie outside our redshift detection range. The image is ﹩9\buildrel{\,\prime}\over{.} 0﹩ across.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: DSS multicolor (IR, red, and blue plates) images of PGC 17124 (center, 30″ white circle). Left: the large white circle shows the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam, and UGC 3276 is denoted by the (60″) cyan circle. The two galaxies with known velocities more than 2000 km s−1 from that of PGC 17124 are denoted by red circles, while the three previously identified galaxies without known velocities are denoted by red crosses. The image is 25′ across. Right: enlargement, showing the disturbed morphology of PGC 17124.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: SDSS DR12 false color (i, r, and g filters) image of the PGC 23328 galaxy group. The white circles show the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam and the ﹩3\buildrel{\,\prime}\over{.} 6﹩ Arecibo beam centered on PGC 2338. The other two known members of the group, WISEA J081955.30+252733.0 and WISEA J081923.48+252621.4, are denoted by cyan circles (listed from left to right in the image). The fourth potential group member, KUG 0816+256B, is denoted by the green circle. The image is 25′ across.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: SDSS DR12 false color (i, r, and g filters) image of our target galaxy PGC 43880 (center, cyan circle). The large white circle shows the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam. The position of SDSS J125405.61+481534.9 is denoted by the red circle, close to our target, while WISEA J125341.21+481813.1 (top center) and WISEA J125257.97+481417.6 (on the right) are denoted by cyan circles. The image is 25′ across.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: DSS false color (IR, red, and blue plates) image of the NGC 2273 galaxy group, which likely includes our target galaxy PGC 95598—inside the large white circle showing the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam. The four other circles denote the known group members, with their color indicating the object’s relative velocity within the group. The image is ﹩110\buildrel{\,\prime}\over{.} 0\times 90\buildrel{\,\prime}\over{.} 0﹩ across
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: SDSS DR12 false color (i, r, and g filters) image of PGC 38698 (center). The large white circle shows the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam. The galaxy I Zw 031 is denoted by the cyan circle on the right and the known background galaxies by red circles. The image is ﹩15^{\prime} ﹩ across.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: SDSS DR12 false color (i, r, and g filters) image of the PGC 30113 galaxy group. The large white circle shows the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam. The six known group members are denoted by cyan circles. The image is ﹩27\buildrel{\,\prime}\over{.} 5﹩ across.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: SDSS DR12 false color (i, r, and g filters) image of PGC 51872 (center, cyan circle). The white circle shows the ﹩3\buildrel{\,\prime}\over{.} 6﹩ Arecibo beam. The yellow circles denote the various galaxies listed in Table 11, which we believe to be part of PGC 51872 rather than separate galaxies.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: SDSS DR12 false color (i, r, and g filters) image of the PGC 32862 galaxy group. The large white circle shows the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam. The four known group members are denoted by cyan circles. The image is ﹩25\buildrel{\,\prime}\over{.} 5﹩ across.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: GBT observations made in a grid around UGC 6179, which indicate that the measured H I gas lies within the central beam. (a) H I spectra measured in each of the the nine ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beams. Please note that the ubiquitous strong, narrow line at ∼13,340 km s−1 is due to RFI. (b) Optical DSS2 blue (Abazajian et al. 2004) image with the nine GBT beams overlaid. (c) SDSS DR12 (Alam et al. 2015) false color (i, r, and g filters) image of UGC 6179 showing the ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beam (green circle) and four known neighbors. The three galaxies with velocities near that of IC 06170 are denoted by white, labeled circles, and the previously unidentified LSB galaxy, [OVS23] 110809.3+635806, is denoted by the cyan circle.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: DSS blue image of UGC 605 showing the ﹩3\buildrel{\,\prime}\over{.} 6﹩ Arecibo and ﹩8\buildrel{\,\prime}\over{.} 7﹩ GBT beams as black circles. The galaxies possibly related to the H I spectra detected when observing UGC 605 are denoted by the cyan circles. Other galaxies are denoted in dark blue and red.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Left: average spectrum of Paloma, without any velocity shift applied. Telluric features have not been removed. Right panels: segments of the average spectra in the donor star’s rest frame, showing a forest of weak metal emission lines from the inner hemisphere. The velocity-corrected spectra are based on the measured semiamplitudes of 220 and 310 km s−1 for the secondary’s inner and outer hemispheres, respectively.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Binned spin profiles of J0846 in 20 nonoverlapping portions of the 6.7-day beat cycle. The top of each panel indicates which beat phases were used to construct each spin profile. The data are repeated along the x-axis for clarity. The pole near spin phase 0.5 has an associated photometric maximum for most of the beat cycle, but it becomes indistinct near beat phase 0.8. Error bars are too small to be visible at this scale.
Paper: Kepler K2 and TESS Observations of Two Magnetic Cataclysmic Variables: The New Asynchronous Polar SDSS J084617.11+245344.1 and Paloma
Authors: Colin Littlefield, D. W. Hoard, Peter Garnavich, Paula Szkody, Paul A. Mason, Simone Scaringi, Krystian Ilkiewicz, Mark R. Kennedy, Saul A. Rappaport, Rahul Jayaraman
Figure caption: Evolution of Paloma’s spin profile across the beat cycle. Beat phase 0.0 occurs when the primary spin maximum coincides with inferior conjunction of the secondary star (i.e., when the spin and orbital phases are both 0.0).
Paper: Constraining the Densities of the Three Kepler-289 Planets with Transit Timing Variations
Authors: Michael Greklek-McKeon, Heather A. Knutson, Shreyas Vissapragada, Daniel Jontof-Hutter, Yayaati Chachan, Daniel Thorngren, Gautam Vasisht
Figure caption: Kepler transit photometry of Kepler-289c. Our initial masks from visual inspection of the transits are shown as gray shading, the final best-fit transit model from the stacked transit profile is overplotted as a blue curve, and our final 3σ outlier masks are shown as red points. We binned the short-cadence data to match the long-cadence data (30 minutes bins) for this figure.