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Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The visible reflectance spectra of irradiated ices 25−30 taken during heating to 320 K. Ices 25−30 in Table 1 are displayed in the order of (a)–(f). All spectra are normalized at 550 nm and plotted as a gradient color from blue to red as temperature increases. Dashed lines represent the spectra of irradiated ices before and after heating to 320 K.
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The visible reflectance spectra of irradiated ices 7−12 taken during heating to 320 K. Ices 7−12 in Table 1 are displayed in the order of (a)–(f). All spectra are normalized at 550 nm and plotted as a gradient color from blue to red as temperature increases. Dashed lines represent the spectra of irradiated ices before and after heating to 320 K.
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The visible reflectance spectra of irradiated ices 1−6 taken during heating to 320 K. Ices 1−6 in Table 1 are displayed in the order of (a)–(f). All spectra are normalized at 550 nm and plotted as a gradient color from blue to red as temperature increases. Dashed lines represent the spectra of irradiated ices before and after heating to 320 K.
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: Colors obtained at different temperatures of (a) 40 K, (b) 20 K, and (c) 10 K. The color of the Sun is labeled with a yellow circle. The gray area is the colors of TNOs from observations (O. R. Hainaut et al. 2012). The colors of methane (13CH4), acetylene (13C2H2), methanol (13CH3OH), and carbon monoxide (13C18O) ices are from previous publications (C. Zhang et al. 2023; C. Zhang et al. 2024). A color threshold is plotted to divide the observed data covered by the colors obtained in laboratory ices from what is uncovered.
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The visible reflectance spectra of ices 31−36 measured during the irradiation. Ices 31−36 in Table 1 are displayed in the order of (a)–(f). All spectra are normalized at 550 nm and plotted as a gradient color from blue to red as radiation dose increases. Dashed lines represent the spectra of ices before and after irradiation.
Paper: A Systematic Analysis of the Radio Properties of 22 X-Ray-selected Tidal Disruption Event Candidates with the Australia Telescope Compact Array
Authors: A. J. Goodwin, M. Burn, G. E. Anderson, J. C. A. Miller-Jones, I. Grotova, P. Baldini, Z. Liu, A. Malyali, A. Rau, M. Salvato
Figure caption: Synchrotron spectral fits for six of the TDEs in the sample with sufficient signal to extract radio spectra at each of the two epochs. The synchrotron model assumes the peak of the radio spectrum is associated with a self-absorption break, as appropriate for a TDE outflow. The spectral model and fitting method are described in Section 4.2.
Paper: A Systematic Analysis of the Radio Properties of 22 X-Ray-selected Tidal Disruption Event Candidates with the Australia Telescope Compact Array
Authors: A. J. Goodwin, M. Burn, G. E. Anderson, J. C. A. Miller-Jones, I. Grotova, P. Baldini, Z. Liu, A. Malyali, A. Rau, M. Salvato
Figure caption: Left: The equipartition radius plotted against time since peak optical or X-ray luminosity for the X-ray-selected sample (colored stars) and the optically selected sample from Y. Cendes et al. (2024; gray points). We find very similar ranges in equipartition radii for the two samples. Right: The equipartition energy plotted against inferred outflow velocity for the X-ray-selected sample (colored stars) and the optically selected sample from Y. Cendes et al. (2024; gray points). We find a marginally statistically significant difference between the equipartition energies of the two samples, with X-ray-selected events tending to have higher outflow equipartition energy for a similar distribution of velocities.
Paper: A Systematic Analysis of the Radio Properties of 22 X-Ray-selected Tidal Disruption Event Candidates with the Australia Telescope Compact Array
Authors: A. J. Goodwin, M. Burn, G. E. Anderson, J. C. A. Miller-Jones, I. Grotova, P. Baldini, Z. Liu, A. Malyali, A. Rau, M. Salvato
Figure caption: The radio luminosity with time since first detection of TDEs in the literature (gray points) and the 22 X-ray-selected TDE candidates in our sample (colored points). 3σ upper limits are indicated by inverted triangles. The luminosity range of the X-ray-selected TDE candidates is consistent with the nonrelativistic TDE population. The literature TDE data are from Y. Cendes et al. (2024), A. J. Goodwin et al. (2022), A. J. Goodwin et al. (2023a), K. D. Alexander et al. (2016), Y. Cendes et al. (2021), A. Horesh et al. (2021a), A. Horesh et al. (2021b), M. M. Anderson et al. (2020), A. J. Goodwin et al. (2023b), J. A. Irwin et al. (2015), and B. A. Zauderer et al. (2011).
Paper: A Systematic Analysis of the Radio Properties of 22 X-Ray-selected Tidal Disruption Event Candidates with the Australia Telescope Compact Array
Authors: A. J. Goodwin, M. Burn, G. E. Anderson, J. C. A. Miller-Jones, I. Grotova, P. Baldini, Z. Liu, A. Malyali, A. Rau, M. Salvato
Figure caption: The 5.5 GHz (no outline) and 9 GHz (black outline) radio lightcurves between the two ATCA epochs of the 22 TDEs in our sample. The sources with statistically significant radio variability are shown as stars, the sources with no statistically significant radio variability are shown in circles, and all nondetections are the 5.5 GHz 3σ upper limits plotted as inverted triangles. The gray stars show additional 5.5 GHz radio data of eRASSt J234403-352641 from A. J. Goodwin et al. (2024). Of the 22 sources in the sample, 11 were radio detected, and eight showed statistically significant radio variability at either 5.5 or 9 GHz.
Paper: A Systematic Analysis of the Radio Properties of 22 X-Ray-selected Tidal Disruption Event Candidates with the Australia Telescope Compact Array
Authors: A. J. Goodwin, M. Burn, G. E. Anderson, J. C. A. Miller-Jones, I. Grotova, P. Baldini, Z. Liu, A. Malyali, A. Rau, M. Salvato
Figure caption: The observed peak 5.5 GHz radio luminosity for the X-ray-selected sample (eROSITA TDEs, green) compared to the optically selected sample (optical TDEs, purple) from Y. Cendes et al. (2024). Note that the peak observed luminosities may not represent the true peak luminosities for each event. We find no statistically significant difference between the peak observed radio luminosity distribution of the two samples.
Paper: A Systematic Analysis of the Radio Properties of 22 X-Ray-selected Tidal Disruption Event Candidates with the Australia Telescope Compact Array
Authors: A. J. Goodwin, M. Burn, G. E. Anderson, J. C. A. Miller-Jones, I. Grotova, P. Baldini, Z. Liu, A. Malyali, A. Rau, M. Salvato
Figure caption: The peak observed 5.5 GHz radio luminosity plotted against the peak observed X-ray luminosity for each of the 22 TDE candidates in the sample. Note that the peak observed luminosities may not represent the true peak luminosities for each event. Each point is colored by the redshift of the host galaxy. Inverted triangles indicate 3σ radio luminosity upper limits. A correlation between the peak radio and X-ray luminosities is apparent, however we caution that there is also a strong distance dependence of this correlation.
Paper: A Systematic Analysis of the Radio Properties of 22 X-Ray-selected Tidal Disruption Event Candidates with the Australia Telescope Compact Array
Authors: A. J. Goodwin, M. Burn, G. E. Anderson, J. C. A. Miller-Jones, I. Grotova, P. Baldini, Z. Liu, A. Malyali, A. Rau, M. Salvato
Figure caption: The fitted synchrotron spectral index, p, for the spectra of the X-ray-selected TDEs (green) and the optically selected sample from Y. Cendes et al. (2024; purple). A KS test indicates a statistically significant difference between the spectral indices of the two samples despite both being fitted allowing the same range of p (2 < p < 4), with X-ray-selected events tending to have higher values of p.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: Comparison with flux densities in the literature. The upper plot shows the distribution of percentage difference, with the horizontal straight line being 0 and the two dashed lines representing ±20. The lower plot compares flux densities, with the diagonal line representing the case where the two are equal. Data in different literature are labeled with different symbols, see the figure legend for details.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: (a) The relationship between the percentage difference in flux and the Hsize parameter (ratio of the H I source area to the beam area). (b) The relationship between the FUMaS flux and the Hsize parameter.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: rms distribution of FAST observations of the UMa region. The black circle marks the UMa region with a radius of 7﹩\mathop{.}\limits^{\unicode{x000B0}}﹩5. The mean value of rms in the region is about 1 mJy beam−1.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: Local group velocity distribution of galaxies in the UMa supergroup. The gray histogram is from FUMaS, the red dashed line is from M. Pak et al. (2014), and the green dotted line is from R. B. Tully et al. (1996).
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: Comparison with H I source location information from previous H I blind survey. HIJASS is marked with “.” and E. Busekool et al. (2021) is marked with “+.” The top histogram shows the distribution of R.A. discrepancies, and the distribution of decl. discrepancies is shown on the right.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: H I column density contours of four small groups overlaid on the DSS B-band optical image. Their integrated ranges are 500–1500 km s−1 for NGC 3992 group (a), 600–1400 km s−1 for NGC 4026 group (b), 500–1300 km s−1 for NGC 4111 group (c), and 550–1500 km s−1 for NGC 3998 group (d), respectively. The contour levels are 6 × 2n × 1018 cm−2 (n = 0, 1, 2, ...). The optical centers of each galaxy are marked as crosses. The HPBW of FAST is indicated at the bottom-left corner of each panel.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: Moment-0 map of the UMa region for the 500–1500 km s−1 integral range. The black circle shows the range of the UMa region. Red circles mark the positions of detections in the FUMaS catalog, with the crosses being the first detected H I sources. The blue crosses are optical galaxies in M. Pak et al. (2014). Boxes mark the positions of the small groups. The size of the marker is proportional to the H I mass and r magnitude.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: Comparison with the 20% (a) and 50% (b) velocity width in the literature. The upper plot of each panel shows the percentage distribution of the difference. Horizontal lines correspond to 0 and ±20, respectively. The lower plot is a comparison of the data, and the corresponding symbols for the different literature data are indicated in the legend. The diagonal line indicates the consistency of the data.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: H I mass and stellar mass distribution of FUMaS detections. The top panel is log(MH I) vs. log(M*), while the bottom is log(MH I/M*) vs. log(M*). The gray dots in the background are FASHI data, and the black line indicates its average distribution. The red crosses are previously detected H I sources, the green dots are new FUMaS detections with known-redshift optical counterparts, and the blue stars are those without known-redshift optical counterparts.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: DESI Legacy Survey’s DR10 multicolor images, moment-0 maps, and profiles for 25 H I sources with optical counterparts without a redshift. The Legacy Survey images are centered on the location of the H I sources and have a range of about 3 × 3 arcmin2. The red circles mark the optical counterparts. The range of the H I sources are indicated in the moment-0 maps. The H I profile plots contain the names of the detections and optical counterparts, the baseline-removed profiles, and the busy-function-fitted profiles.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: Moment-0 map of NGC 3877 and UGC 7218. The outer black contour is the ellipse size of the source. The inner blue line is the contour with column density 5 × 1019 cm−2. The H I position of the source and the HPBW of FAST are marked in the plot.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: Similar to Figures 4 and 5(a), except that the flux densities of the FUMaS detections are for the region of column densities exceeding 5 × 1019 cm−2.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: The top panel shows the H I MF of the UMa supergroup. The gray points with error bars are the number densities within each bin. The curve fitted by the MML method is the blue solid line, with the 1σ uncertainty in the blue area. The red dashed line is the best fit from the LMFIT package based on the NLLS method. The result in E. Busekool et al. (2021) is shown with the green dotted line. The lower panel shows a histogram of the galaxy number distribution.
Paper: The FAST Ursa Major Supergroup H I Survey (FUMaS): Catalog and H I Mass Function
Authors: Haiyang Yu, Ming Zhu, Chuan-Peng Zhang, Peng Jiang, Jin-Long Xu
Figure caption: The H I MF calculated with the NLLS method in different cases: (a) excluding H I clouds and filaments, dividing small groups and confused pairs into individual galaxies; (b) including H I clouds and filaments, dividing small groups and confused pairs into individual galaxies; (c) excluding H I clouds, not dividing small groups and confused pairs into individual galaxies; (d) including H I clouds, not dividing small groups and confused pairs into individual galaxies.
Paper: Hemispheric Distribution of Solar Active Regions during Solar Cycles 23–25
Authors: Yuxia Liu, Tingting Xu, Miao Wan, Linhua Deng, Xinhua Zhao, Shiyang Qi, Nanbin Xiang, Weihong Zhou
Figure caption: Time evolution of the AR parameters from 1996 May to 2023 November. From top to bottom: AR number, area, and flux. The blue (red) lines represent the northern (southern) hemisphere. The black (gray) dashed lines represent the maximum and minimum times of the solar cycles.
Paper: Hemispheric Distribution of Solar Active Regions during Solar Cycles 23–25
Authors: Yuxia Liu, Tingting Xu, Miao Wan, Linhua Deng, Xinhua Zhao, Shiyang Qi, Nanbin Xiang, Weihong Zhou
Figure caption: Butterfly diagrams of AR parameters from 1996 May to 2023 November. From top to bottom, the panels depict the latitude–time distribution of AR number, area, and flux. The colors show AR number, average area, and flux, respectively.
Paper: Hemispheric Distribution of Solar Active Regions during Solar Cycles 23–25
Authors: Yuxia Liu, Tingting Xu, Miao Wan, Linhua Deng, Xinhua Zhao, Shiyang Qi, Nanbin Xiang, Weihong Zhou
Figure caption: Panel (a): cumulative asymmetry in the AR parameters across different hemispheres during SC23. The red and blue lines indicate an excess in the cumulative sum between the southern and northern hemispheres. Panels (b), (c), and (d) are similar to panel (a), corresponding to SC24, SC25, and the entire time period, respectively.
Paper: Calibrating HMI Magnetograms Using an End-to-end Magnetograph Model
Authors: Gordon J. D. Petrie, Julián Blanco Rodríguez, Valentín Martínez Pillet, Han Uitenbroek, Philip H. Scherrer
Figure caption: Maps of the emergent continuum intensity IC computed by the RH code from the MURaM simulation data cube simulating four viewing angles, 0°, 41﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4, 60°, and 75﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5. Limb-darkening is reproduced by the decrease in quiet-Sun continuum intensity with increasing viewing angle. The labeled regions representing umbral, plage, and quiet-Sun pixels are chosen for analysis later in the paper—see the text for details.
Paper: Calibrating HMI Magnetograms Using an End-to-end Magnetograph Model
Authors: Gordon J. D. Petrie, Julián Blanco Rodríguez, Valentín Martínez Pillet, Han Uitenbroek, Philip H. Scherrer
Figure caption: Maps of the amplitude (normalized by IC) of Stokes V, taken at its maximum value shortward of nominal line center in each pixel. This quantity is mapped for the same viewing angles as in Figure 1, and is a signature of the LOS magnetic field. The apparent polarity change at the far side of the umbra and penumbra for slanted viewing angles is due to these fields being tilted with respect to local vertical. The labeled regions representing umbral, plage, and quiet-Sun pixels are chosen for analysis later in the paper—see the text for details.
Paper: Calibrating HMI Magnetograms Using an End-to-end Magnetograph Model
Authors: Gordon J. D. Petrie, Julián Blanco Rodríguez, Valentín Martínez Pillet, Han Uitenbroek, Philip H. Scherrer
Figure caption: Magnetic field map derived from the MHD simulation data cube for the same viewing angles as in Figure 1. For each viewing angle, the pixel values are averages along the LOS, weighted by the RH contribution functions. The maps therefore represent the magnetic field at the HMI line formation heights, and form a ground-truth reference for the SOPHISM HMI simulation results that follow.
Paper: Calibrating HMI Magnetograms Using an End-to-end Magnetograph Model
Authors: Gordon J. D. Petrie, Julián Blanco Rodríguez, Valentín Martínez Pillet, Han Uitenbroek, Philip H. Scherrer
Figure caption: Map of mean heights derived from the contribution functions for the same viewing angles as in Figure 1. For each viewing angle, the pixel values are height averages along the LOS weighted by the RH contribution functions. The maps therefore represent the weighted mean HMI line formation height, which is used to form the ground-truth reference magnetograms shown in Figure 3. The zero-point of the color scale represents the center of the range of line formation height values.
Paper: Calibrating HMI Magnetograms Using an End-to-end Magnetograph Model
Authors: Gordon J. D. Petrie, Julián Blanco Rodríguez, Valentín Martínez Pillet, Han Uitenbroek, Philip H. Scherrer
Figure caption: Scatter plots of BMHD against BHMI for the four viewing angles, 0° (top row), 41﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4 (second row), 60° (third row), and 75﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 (bottom row); and for different classes of field, all fields (first column), umbral (second column), penumbra (third column), and quiet Sun (fourth column). Because the MHD magnetic field data set has such a strong positive-polarity bias, we use the combined polarity-symmetric data set ±BMHD and ±BHMI to derive the symmetric calibration curves that appear as black curves in the second, third, and fourth columns. In this figure, we only show the cases of BHMI with zero spacecraft velocity as an illustrative example, and we follow the same procedure for a range of nonzero spacecraft velocities as described in the text.
Paper: Calibrating HMI Magnetograms Using an End-to-end Magnetograph Model
Authors: Gordon J. D. Petrie, Julián Blanco Rodríguez, Valentín Martínez Pillet, Han Uitenbroek, Philip H. Scherrer
Figure caption: Comparison of RH (red solid lines) and SOPHISM (red filled circles) wavelength-dependence with observational data from the disk-center FTS atlas (blue dotted line) and HMI Stokes I data (green filled squares). The RH, SOPHISM, and HMI data are shown for all four viewing angles, and the disk-center FTS data only for 0°. Also shown as yellow-orange brackets for all viewing angles are continuum intensity values derived from the observed wavelength dependence of limb-darkening obtained at the McMath Solar Telescope by A. K. Pierce & C. D. Slaughter (1977, PS77). The RH values are based on the labeled strips of representative quiet-Sun pixels from the MHD data cube shown in Figure 1, and the SOPHISM values from averages over equivalent strips of representative quiet-Sun pixels in the SOPHISM output data sets for zero spacecraft velocity. The HMI observational values are derived from quiet-Sun central-meridian Stokes I measurements from 2015 April 22 with the respective heliocentric angular positions. The RH and FTS data are presented in physical units, emphasizing the excellent match, in intensity and line shape, between the 0° RH profile and the disk-center FTS profile. Every other quantity is normalized by its disk-center (0°) continuum value IC.
Paper: Calibrating HMI Magnetograms Using an End-to-end Magnetograph Model
Authors: Gordon J. D. Petrie, Julián Blanco Rodríguez, Valentín Martínez Pillet, Han Uitenbroek, Philip H. Scherrer
Figure caption: Plot of radial magnetic flux against time for a quiet-Sun region over the 3 days 2015 April 21–23. This region was located at the center of the disk at 12:00 on April 23, indicated by the dotted boxes of size 10° × 10° at the disk-center in each panel of Figure 12, and was tracked back and forward in time using the equatorial surface rotation rate. The radial flux was calculated using three magnetogram sources: (1, dashed line) for the regular 12 minute HMI LOS magnetograms as distributed via JSOC; (2, dotted line) equivalent 12 minute magnetograms derived by us from the HMI Stokes I and V data available from JSOC, using the usual HMI LOS magnetic field formula (S. Couvidat et al. 2012a); and finally (3, solid line) calibrated magnetograms produced by us by applying the look-up tables to data set (2). The middle panel shows the relative variation ﹩({F}_{r}-\bar{{F}_{r}})/| \bar{{F}_{r}}| ﹩ over this time. The bottom panel plots the SDO spacecraft radial orbital velocity against time.