adsabs/AstroCLIMB huggingface dataset:
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Flare area vs. flare energy (top) and flare temperature (middle). The horizontal dashed line corresponds to the area of one solar hemisphere. The red line in the top panel shows the linear fit to the data. The bottom panel shows the flare energy divided by flare area, in cgs units, vs. flare temperature. The red dashed line shows the fit to all points. The solid red line shows a fit to flares with ﹩{T}_{\mathrm{flare}}\,\lt ﹩ 10,000 K. The blue dotted horizontal line is the weighted mean for flares with ﹩{T}_{\mathrm{flare}}\,\gt ﹩ 10,000 K. The flare temperature uncertainties were omitted in the middle and bottom panels for a better visualization.
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Weighted mean flare temperature, ﹩{\bar{T}}_{\mathrm{flare}}﹩(k), as in Figure 6 (first row), for stars with six or more flares. The CoRoT ID and stellar spectral type are shown in each panel. The vertical dashed lines on four of the stars separate the flares obtained in different observation sequences: during 2008 and 2012. The vertical axis range is twice as large for the first three stars as for the others.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Ratio of the measured and the theoretically expected noise as a function of the exozodi level for the 10 pm rms WFE, 10 pc case (top row), the 30 pm rms WFE, 10 pc case (second row), the 90 pm rms WFE, 10 pc case (third row), the 10 pm rms WFE, 15 pc case (fourth row), and the LUVOIR-B, 10 pc case (bottom row). Shown is the average over 200 simulated observations of solar system twins with inclinations of 0 deg (left column), 30 deg (middle column), and 60 deg (right column). The blue curve shows the reference star subtraction case, the orange curve shows the 10/20 deg roll subtraction case, and the green curve shows the 180 deg roll subtraction case. In the top row, the dashed lines show the simulations including detector noise which were only computed up to 100 zodi due to exceedingly long computation times.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Simulated coronagraphic images of the solar system with 10 zodi of warm dust, at 60 deg inclination, and at a distance of 10 pc together with the best-fit parametric disk models. Red represents positive counts and blue represents negative counts, both shown in a logarithmic color stretch. The reference star or roll-subtracted images are shown in the left column, the best-fit parametric disk models are shown in the middle column, and the residuals are shown in the right column. The top row shows the reference star subtraction, the middle row shows the 10 deg roll subtraction, and the bottom row shows the 180 deg roll subtraction case. The symmetry (solid green lines) and antisymmetry (dashed green lines) axes of the parametric disk models are highlighted in the middle column and the locations of the Earth twin are highlighted by solid green (science image) and dashed green (roll image) circles in the right column. The integration time is chosen to detect the Earth twin at a photon noise-limited S/N of 7 in the roll subtraction case and equals 1048 s.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Noiseless coronagraphic scene image obtained by convolving the exoVista scene with the LUVOIR-A APLC PSF (left panel) and the same image with photon noise added and downsampled to a detector pixel scale of 4.77 mas (right panel). The image shows the contribution of the companions, the exozodiacal dust disk, and stellar speckles behind the coronagraph for a 60 deg inclined solar system with 10 zodi of dust and at a distance of 10 pc. The position of the host star (here, the Sun) is indicated by a black star and the position of the planetary-mass companion (here, the Earth) is indicated by a green circle. It can be seen that one obtains less than one photon per second from an Earth twin at a distance of 10 pc and a wavelength of 500 nm observed through an 18% bandpass (assuming a total system throughput of ∼31.78%).
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Schematic illustrating the different PSF and disk subtraction methods used in this work. We start by simulating coronagraphic images of a PSF reference (REF) and the science target (SCI 1) as well as the science target with a roll angle of 10/20 and 180 deg (SCI 2). Then, we perform reference star or roll subtraction to calibrate stellar speckles and subsequently subtract a best-fit toy model for the residual exozodiacal disk flux from the images. In the resulting science products (disk and antisymmetric subtraction), we then measure the residual noise and compare it to the theoretical photon and detector noise limit.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Distribution of the best-fit inclination retrieved from the fits with free inclination. The true system inclination is highlighted by a dashed black line. For each scenario, 200 individual fits were performed with the prior of the inclination i being randomly distributed so that ﹩\cos (i)\in [-1,1)﹩.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Histograms of the measured pixel-to-pixel noise distribution in the 200 simulated observations of solar system twins with inclinations of 0 deg (left column), 30 deg (middle column), and 60 deg (right column), exozodi levels from 1 to 1000 zodi (top to bottom row), and at a distance of 10 pc. The blue histograms show the reference star subtraction case and the orange and green histograms show the 10 and 180 deg roll subtraction cases. The solid and dashed vertical lines show the theoretically expected and the mean of the empirically measured noise, respectively.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Same as Figure 6, but for the vector vortex charge six coronagraph used for the LUVOIR-B simulations.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: Top row: these panels present the PV diagrams of the line ratios He I λλ4713/4026 (left), He I λλ4713/4471 (middle), and He I λλ4713/5876 (right). The contours show the intensity of the He I λλ4026, 4471, and 5876 lines (the denominator of the ratio). Middle row: these panels present various statistics for the ratios of the PV diagrams of He I λλ4713/4026 (left), He I λλ4713/4471 (middle), and He I λλ4713/5876 (right) as a function of the line intensities in the original PV diagrams of the He I λλ4026, 4471, and 5876 lines (denominator). In the top and middle rows, the line ratios have been corrected for the flux scale factors (Table 5), but not for reddening. Bottom row: these panels compare the ratio of the line intensities of He I λλ4713/4026 (left), He I λλ4713/4471 (middle), and He I λλ4713/5876 (right), now corrected for reddening (Table 6), with the theoretical line intensities from Porter et al. (2013). We adopt the mean line ratio for all pixels exceeding 30% of the maximum line intensity of the denominator and the uncertainty given by the standard deviation. The He I lines are compatible with temperatures ﹩\mathrm{log}{T}_{e}=3.91\mbox{--}4.07﹩ when considering densities up to 104 cm−3 (see Figure 22).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: Top row: these panels present the PV diagrams of the line ratios He I λλ4026/5876 (left) and He I λλ4471/5876 (right). The contours show the intensity of the He I λ5876 line (the denominator). Middle row: these panels present various statistics for the line ratios of He I λλ4026/5876 (left) and He I λλ4471/5876 (right) as a function of the line intensities in the original PV diagram of the He I λ5876 line (denominator). These line ratios have been corrected for the flux scale factors (Table 5), but not reddening. Bottom row: these panels compare the ratio of the lines of He I λλ4026/5876 (left) and He I λλ4471/5876 (right), now corrected for reddening, with the theoretical line intensities from Porter et al. (2013). These line ratios are insensitive to temperature, but have some sensitivity to density and are useful to check the reddening (Table 6). These He I lines are compatible with densities up to 104 cm−3.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: Left: we present the temperature-sensitive N II λλ4041/5680 ratio and its uncertainty (the pink region), based upon an intensity limit at 40% of the maximum intensity and the 90% width of the distribution of pixel values. This ratio is corrected for both reddening and the scale factor between the CD2 and CD3b wavelength intervals. T  e  > 2000 K if the electron density is very low; T  e  > 5000 K for higher densities. Right: we present the density-sensitive N II λλ5666/5680 ratio and its uncertainty (the pink region; same definitions). The N II λλ5666/5680 ratio is compatible with high densities (3000 − 105 cm−3) and a wide range of electron temperatures (500−16000 K).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams for the lines (left) of N II λ4041, N II λ5666, and N II λ5680, and for the line ratios (right) N II λλ4041/5680 and N II λλ5666/5680. The contour lines are of the N II λ5680 intensity. The spatial coverage of the PV diagram of N II λ4041 is less than that for the others. Both the temperature- and density-sensitive maps (4041/5680 and 5666/5680, respectively) are reasonably uniform.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams of the [S II] λλ6716,6731 lines and of the [S II] density. In all panels the contours are of the [S II] λ6716 line intensity. The white color in the PV diagram of the [S II] density represents nonphysical values or where there is no [S II] emission. The color scale for the density spans the range 0–10, 000 cm−3.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams of the [Cl III] λλ5717,5537 lines and of the [Cl III] density. In all panels, the contours are of the [Cl III] λ5717 line intensity. The white color in the PV diagram of the [Cl III] density represents nonphysical values or where there is no [Cl III] emission. The color scale for the density spans the range 0−10,000 cm−3.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams for the lines of [Ar IV] λλ4711,4740 and of the [Ar IV] density. In all panels, the contours are of the intensity of the [Ar IV] λ4711 line. The white color in the PV diagram of the [Ar IV] density represents nonphysical values or where there is no [Ar IV] emission. The color scale for the density spans the range 0–10, 000 cm−3.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the intensities of reddening-corrected, high-n Paschen lines with respect to the intensity of Hβ as a function of the upper level for assumed electron temperatures of 1000 K (left) and 10,000 K (right). The implied densities are of ∼1000 cm−3 at 1000 K and perhaps ∼10,000 cm−3 at 10,000 K.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the intensities of reddening-corrected, high-n Balmer lines with respect to the intensity of Hβ as a function of the upper level for assumed electron temperatures of 1000 K (left) and 10,000 K (right). The implied densities are between <1000 cm−3 and ∼10,000 cm−3.
Paper: Mass–Velocity Dispersion Relation by Using the Gaia Data and Its Effect on Interpreting Short-duration and Degenerate Microlensing Events
Authors: Sedighe Sajadian, Sohrab Rahvar, Fatemeh Kazemian
Figure caption: The scale parameter vs. ﹩1/\sqrt{\left\langle M\right\rangle }﹩ (in units of the solar mass) for different subsamples with different mass ranges (green points). The best-fitted linear and power-law lines, given by Equations (3) and (4), are shown by dashed and dotted lines, respectively.
Paper: Mass–Velocity Dispersion Relation by Using the Gaia Data and Its Effect on Interpreting Short-duration and Degenerate Microlensing Events
Authors: Sedighe Sajadian, Sohrab Rahvar, Fatemeh Kazemian
Figure caption: The velocity profiles for different stellar masses detected by the Gaia telescope. For each profile, an MB distribution is fitted to data that is shown by a magenta dashed curve. Two curves that restrict the filled magenta area represent MB distributions with the scale parameters a ± σ  a . The parameters of the best-fitted MB curves are reported in Table 1.
Paper: Mass–Velocity Dispersion Relation by Using the Gaia Data and Its Effect on Interpreting Short-duration and Degenerate Microlensing Events
Authors: Sedighe Sajadian, Sohrab Rahvar, Fatemeh Kazemian
Figure caption: The normalized distribution of the Einstein crossing time (left panel) and the lens–source relative velocity (right panel) of simulated microlensing events. In the simulation for each lensing configuration, the lens–source relative velocity and the Einstein crossing time are calculated by considering the MVR (black step distributions) and without applying it (filled light-green ones).
Paper: Mass–Velocity Dispersion Relation by Using the Gaia Data and Its Effect on Interpreting Short-duration and Degenerate Microlensing Events
Authors: Sedighe Sajadian, Sohrab Rahvar, Fatemeh Kazemian
Figure caption: The luminosity–temperature diagram of stars in our sample, as reported in the Gaia DR3. Main-sequence and giant stars are specified by red triangles and green circles, respectively.
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: All of the signals above an S/N of 10 detected at the first filter threshold (any signal above the S/N detected in any ON source pointing) of turboSETI in the L band. Each signal is sized by the log of the S/N. The drift rates of each signal are determined by the turboSETI algorithm. Hits passing only the first filter threshold (any signal above the S/N detected in any ON source pointing) are marked as blue dots. The purple triangles indicate hits passing the second filter threshold (any signal above the S/N in at least one ON and no OFF source windows). The golden stars indicate the hits that passed the third filter threshold (signal detection in all ONs and no OFFs). The orange dashed lines correspond to the barycentric drift rates, of −0.124, −0.125, and −0.127 Hz s−1, for each of the three ON source pointings. The faint blue vertical stripes correspond to signals within 1.87 MHz (0.1% of the maximum frequency in this band) of each other, likely indicating they are part of an RFI comb. Data outside regions of detector sensitivity as well as those falling within the notch filter (1.25–1.35 GHz) have been grayed out.
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: All of the signals above an S/N of 10 detected at the first filter threshold (any signal above the S/N detected in any ON source pointing) of turboSETI in the S band. Each signal is sized by the log of the S/N. The drift rates of each plotted point, corresponding to a signal above the S/N, are determined by the turboSETI algorithm. Hits passing only the first filter threshold (any signal above the S/N detected in any ON source pointing) are marked as blue dots. The purple triangles indicate hits passing the second filter threshold (any signal above the S/N in at least one ON and no OFF source windows). The golden stars indicate the hits that passed the third filter threshold (signal detection in all ONs and no OFFs). The orange dashed line corresponds to the barycentric drift rate, of −0.18 Hz s−1, for each of the three ON source pointings. The light blue vertical strips correspond to signals within 2.8 MHz (0.1% of the maximum frequency in this band) of each other, likely indicating they are part of an RFI comb. Data outside regions of detector sensitivity as well as those falling within the notch filter (2.30–2.36 GHz) have been grayed out.
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: The single L-band hit that passed turboSETI’s strictest filtering threshold, intended to select for narrowband signals that appear in every ON source pointing and none of the OFF source pointings, in the target drift rate range near −0.124 Hz s−1. Each rectangular block labeled “ON_L” and “OFF_HD13908” stacked on top of each other shows the ON/OFF observation cadence. This is plotted over a narrow frequency range of 602 Hz centered at the detected signal frequency of 1626.076447 MHz. The red dashed line indicates turboSETI’s best-fit drift rate for this signal. The color mapping indicates power, normalized to the maximum power in each panel. It is difficult to determine what turboSETI picked up from this plot alone, but Figure 7 shows that it is RFI with a bandwidth of ∼80 kHz. Many hits in turboSETI show similar features, where a zoomed-out look clarifies that the signal is drifting RFI.
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: All of the signals above an S/N of 10 detected using the turboSETI algorithm around the barycentric drift rates, between −0.124 and −0.127 Hz s−1 in the ON target pointings, for these observations in the L band. This shows the S/N for all the hits around the dashed orange lines shown in Figure 4 within the detector sensitivity range. Hits passing only the first filter threshold (any signal above the S/N detected in any ON source pointing) are marked as blue dots. The purple triangles indicate hits passing the second filter threshold (any signal above the S/N in at least one ON and no OFF source windows). The lone golden star indicates the one hit within this drift rate window that passed the third filter threshold (signal detection in all ONs and no OFFs). Figure 6 shows the dynamic spectrum of this signal.
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: Zoomed-out plot of Figure 6, covering more than 80 kHz in the L band (as compared to 602 Hz in the previous plot). The red box indicates the plot window in Figure 6. From this plot it is easier to see what the algorithm likely picked up as a potential signal. This shows our most promising result is simply an RFI signal.
Paper: A Search for Radio Technosignatures at the Solar Gravitational Lens Targeting Alpha Centauri
Authors: Nick Tusay, Macy J. Huston, Cayla M. Dedrick, Stephen Kerby, Michael L. Palumbo III, Steve Croft, Jason T. Wright, Paul Robertson, Sofia Sheikh, Laura Duffy, Gregory Foote, Andrew Hyde, Julia Lafond, Ella Mullikin, Winter Parts, Phoebe Sandhaus, Hillary H. Smith, Evan L. Sneed, Daniel Czech, Vishal Gajjar
Figure caption: All of the signals above an S/N of 10 detected using the turboSETI algorithm around the barycentric drift rates, of −0.18 Hz s−1, for these observations in the S band. This shows the S/N for all the hits around the dashed orange lines shown in Figure 8 within the detector sensitivity range. Hits passing only the first filter threshold (any signal above the S/N detected in any ON source pointing) are marked as blue dots. The purple triangles indicate hits passing the second filter threshold (any signal above the S/N in at least one ON and no OFF source windows). No hits within this drift rate window passed the third filter threshold (signal detection in all ONs and no OFFs).