adsabs/AstroCLIMB huggingface dataset:
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption: The Moon’s orbital period over time (blue dashed and solid lines) and the maximum inclination of the moon planet relative to the star or a distant observer (red dashed and solid lines) for a mutual events to occur every moon orbit. We used tidal evolution models to derive the orbital period at early times, and the Moon’s orbital evolution at older ages was taken from (Farhat et al. 2022).
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption: An illustration of mutual events in an aligned moon–planet–star system viewed by an edge-on observer.
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption:  Left-hand panel: Number of transits or shadow events required to detect (with a 5-σ confidence level) a Moon analog around an Earth-analog planet in 39 nearby star systems (circles) in the 550 nm band, and the best fit to the simulations (black line). For the nearest systems, Moon analogs are detectable with observation of just two shadow or transit events. The simulated systems leverage results from the LUVOIR-B concept in The LUVOIR Team (2019). Right-hand panel: Number of transits or shadow events required to detect a moon with mass 0.01M p  (black; our Moon is 0.01M⊕) or 0.1M p  (red) around a planet that is 1.0 R ⊕ (solid lines) or 1.5 R ⊕ (dashed lines). In the most favorable cases, large moons of terrestrial worlds will remain detectable with <10 shadow or transit detections out to 20 pc. Eclipse or occultation events are 10×harder to detect at this wavelength, but become much more amenable to detection at longer wavelengths (see Figure 6).
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption: Number of eclipse or occultation events required to detect (with a 5-σ confidence level) a Moon analog around an Earth-analog planet in 37 nearby star systems (circles) in the 1.4 μm spectral band, and the best fit to the simulations (black line). For the nearest systems, Moon analogs are detectable with observation of just a few eclipse or occultation events. In this spectral band, eclipse or occultation events can be detected with half the number of shadow or transit events that would be required for detection. We leverage of the simulated systems results from the LUVIOR-B concept in The LUVOIR Team (2019).
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption: Detectability of exomoon transits in the 850 nm light curve with Earth’s variability included in the light curve (blue line; same as the dash-dotted blue line in Figure 10) and with Earth’s variability removed (gray line). In the case with variability removed, the moon remains detectable, even as the photometric precision worsens (goes up). For our Earth–Moon system and at 850 nm, this demonstrates that the detectability of our moon is limited primarily by host variability rather than photon noise. In other spectral bands or for larger moons that produce much larger transits than planet variability amplitudes, photon noise will be the primary limitation in moon detection.
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption:  Left-hand Axis (blue lines): Percentage of detected Moon transits as a function of photometric precision in the simulated light curves using the EPOXI data. Transits are more difficult to detect at 450 nm and 850 nm due to the structure of the Earth’s variability in those spectral bands. Right-hand Axis (red line): Theoretical S/N, from Equation (6), in the photon-noise limit.
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption:  Left-hand panel: An example of simulated data (gray errorbars) based on the EPOXI light curve measurement (black line) at 550 nm with a simulated photometric precision of 4% per 15 minutes (1.5% precision for the full transit duration). The GP+transit fit (red line) and transit only fit (blue dotted line; from the GP+transit fit) is also plotted. Right-hand panel: Corner plot from GP+transit fit showing the mid-time of transit (T0), the transit depth (δ), the transit duration (D), and the slope of ingress/egress.
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption: Still frame of the Moon transit during NASA EPOXI mission observations of Earth. Video link: https://epoxi.astro.umd.edu/3gallery/vid_Earth-Moon.shtml; Video Credit: Don J. Lindler, Sigma Space Corporation and NASA/JPL-Caltech/GSFC/UMD.
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption: The photometric precision (ppt) per hour on an Earth-analog in the habitable zone of 39 nearby systems observed with LUVOIR-B in the 550 nm coronagraphic band. Photometric precisions are based on the calculations in (The LUVOIR Team 2019).
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption: Measured light curves of the Moon transiting in front of the Earth as observed by the NASA EPOXI mission.
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Magnitude distribution of all detected and new sources from this work compared to L20 and D23. Also shown are sources detected only in previous studies in M31 Field 13 and SMC. Top-left panel: M31 Field 13 PHAT survey overlapping region in FUVCaF2 filter compared with L20 (Leahy et al. 2020). Top-right panel: M31 Field 13 PHAT survey overlapping region in NUVN2 filter compared with L20. Bottom-left panel: SMC in FUVBaF2 filter compared with D23 (Devaraj et al. 2023a). Bottom-right panel: SMC in NUVB13 filter compared with D23.
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Regions used for comparison in this work. Left panel: UVIT observation of M31 Field 13 in NUVN2 filter. White dashed circles represent the central 12′ region, and green boxes represent the PHAT survey overlapping regions. Right panel: UVIT observations of three partially overlapping MC regions in the NUVB13 filter. Red, green, and blue correspond to SMC1, SMC2, and SMC3 fields, respectively. The inner dashed circle corresponds to the central 12′ regions of each field used in the current analysis.
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Histogram of UVIT background distribution in 128 × 128 pixel source-free region compared with the expected Poisson and Gaussian distribution in the field of M31 Field 13 NUVN2 filter.
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Ratio of 3σ equivalent threshold from Gaussian and Poisson distribution as a function of background counts.
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Left panel: Log(N) vs. Log(S) plot in the FUVBaF2 filter of the GOODS-N field for detected sources in this work at 4, 3 and 2σ equivalent threshold and sources detected in Mondal et al. (2023). A straight line of slope 1.5 is plotted as a reference. Right panel: zoomed-in image of Figure 9 showing the magnitude limits reached at different thresholds.
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Log(N) vs. Log(S) plot in the NUVB13 filter of the SMC field for sources detected in this work and sources detected in D23 (Devaraj et al. 2023a). A straight line of slope 1.5 is plotted as a reference. The improvement in the identification of fainter sources is clearly visible.
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Color–magnitude diagram for sources detected in both FUV and NUV having counterparts in previous UVIT studies compared with new sources detected in both FUV and NUV of this work. Left panel: in M31 Field 13 compared with L20 (Leahy et al. 2020). Right panel: in SMC compared with D23 (Devaraj et al. 2023a).
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Gaia G magnitude in NUVB13 filter of SMC field for sources NUVB13 magnitude less than 22 (dotted) and greater than 22 (dashed–dotted).
Paper: Detection of Faint Sources by the UltraViolet Imaging Telescope Onboard AstroSat Using Poisson Distribution of Background
Authors: B. Ananthamoorthy, Debbijoy Bhattacharya, P. Sreekumar, Swathi B
Figure caption: Completeness of the catalog as a function of magnitude in the field of SMC.
Paper: Speckle Interferometry at SOAR Telescope in 2023
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Magnitude difference Δm vs. separation ρ for pairs measured in 2023 (crosses). The upper axis indicates periods of binaries with such separations and a mass sum of 1 ﹩{{ \mathcal M }}_{\odot }﹩ if located at 100 pc distance. The hatched area highlights expected future measurements from Gaia, and the vertical dotted line shows the SOAR diffraction limit in the I band.
Paper: Speckle Interferometry at SOAR Telescope in 2023
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Six new visual orbits with well-constrained orbital elements. In each plot, the ellipse shows the fitted orbit, and squares connected to the ellipse are accurate speckle data, while visual measures and nonresolutions are shown as crosses. The primary component (asterisk) is at coordinate origin; the axis scale is in arcseconds. Orientation, periods, semimajor axes, and sense of rotation are indicated.
Paper: Speckle Interferometry at SOAR Telescope in 2023
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Three combined spectro-interferometric orbits. The upper plots are similar to those in Figure 2; the corresponding RV curves are shown below.
Paper: Speckle Interferometry at SOAR Telescope in 2023
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Orbits of four inner pairs in nearby hierarchical systems. The axis scale is in arcseconds.
Paper: Speckle Interferometry at SOAR Telescope in 2023
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Fragments of speckle autocorrelation functions (ACFs) of three newly identified compact hierarchies within 100 pc (in arbitrary negative rendering). Outer and inner separations are indicated, and the ACF peaks corresponding to true companion locations are labeled.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: Selection of AGNs (z < 0.3) with powerful outflows and very high optical continuum luminosity from the SDSS type 1 AGNs (Rakshit & Woo 2018). Gray dots indicate the SDSS sample. Top panel: distribution of log ﹩{\sigma }_{[\mathrm{OIII}]}^{{\prime} }﹩ as a function of optical continuum luminosity at 5100 Å. The black dashed line indicates L5100Å > 1043.5 erg s−1. Bottom left panel: the distribution of log ﹩{\sigma }_{[\mathrm{OIII}]}^{{\prime} }/{M}_{* }^{1/4}﹩ is displayed as a function of L5100Å normalized by stellar mass (M *;  from the MPA-JHU catalog). Note that ﹩{{\rm{M}}}_{* }^{1/4}﹩ is a proxy for stellar velocity dispersion. The black dashed and dotted lines represent L 5100 Å/M * > 1033.5 and ﹩\mathrm{log}\ {\sigma }_{[\mathrm{OIII}]}^{{\prime} }/{M}_{* }\ \gt \ 0﹩ (indicating high luminosity and powerful outflows), respectively. There are 32 targets (red and blue points) that satisfy these criteria. Purple stars indicate targets that have been observed and are available in the SCUBA-2 submillimeter archival data. Bottom right panel: a zoomed-in view of the left panel for a detailed look at our selected sample (red points). Interestingly, one of our selected targets exhibits extremely high continuum luminosity and outflow strength properties (L 5100 Å/M * > 1033.8 and ﹩\mathrm{log}\ {\sigma }_{[\mathrm{OIII}]}^{{\prime} }/{M}_{* }\ \gt \ 0.15﹩, represented by green dashed and dotted lines, respectively).
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: Selection of AGNs (z < 0.3) with powerful outflows and high radio luminosities from the SDSS type 1 AGNs (Rakshit & Woo 2018). Gray dots indicate the SDSS sample. Points with red circles represent our 21 selected objects in the proposals M22BP083 and M23AP023, respectively. Left panel: distribution of outflow velocity ﹩{\sigma }_{[\mathrm{OIII}]}^{{\prime} }﹩ as a function of radio luminosity. Right panel: distribution of log ﹩{\sigma }_{[\mathrm{OIII}]}^{{\prime} }/{M}_{* }^{1/4}﹩ as a function of radio luminosity normalized by stellar mass. Note that ﹩{M}_{* }^{1/4}﹩ serves as a proxy for stellar velocity dispersion. The vertical dashed line and horizontal dotted line denote L 1.4GHz/M *  > 1029.5 erg s−1 and log ﹩{\sigma }_{[\mathrm{OIII}]}^{{\prime} }﹩/M * 1/4 ≳  −0.4 (indicating powerful radio jets and outflows), respectively. The gray dots without red circles within the threshold green lines on the top right portion of the right panel denote data available in the JCMT archive.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: An integrated DBSP spectrum of J0749+4510 (z = 0.192, m r = 16.78 mag). We fitted the spectrum using the BADASS package (Sexton et al. 2020). Top panel: the observed spectrum (black) and fitting models, including AGN power-law continuum (purple); Balmer continuum (cyan); Fe II emission (magenta); and narrow (green) and broad (pink) emission line models. The shaded region around the 6100 Å continuum is discarded from the spectral fitting. Bottom panels: the fitting models of emission lines show multiple broad and narrow components in their profiles, e.g., Mg II, Hβ, [O III], and Hα. The high S/N spectrum with detected multiple emission lines gives us great interest in exploring the ionized gas kinematics along the long slit.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: SED fitting results of two targets in our proposals. The text in the figures provides explanations for the models and data points. For both of these targets, the SEDs, ranging from UV to MIR bands, are dominated by AGN emission, while the FIR/submillimeter SEDs primarily result from dust reemission. Therefore, the utilization of SCUBA-2 is crucial for accurately estimating the SFRs of our targets. The triangle indicates the upper limit of detection.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: Comparison of SFRs determined from SED fittings with and without including JCMT data. The red and gray solid lines show the best fits for sources with detected and upper limit detections in the JCMT data, respectively. The dashed line displays the one-to-one relation.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: Spatially resolved spectra of J0749+4510 (z = 0.192, m r = 16.78 mag) obtained with DBSP. In the top left panel, we present the S/N at the 5100 Å continuum as a function of position along the slit direction. On the top right, we show the measured velocities of the Hβ narrow component varying along the slit direction. The bottom panels display the extracted spectra of the Hβ and [O III] emission lines at 4969 Å and 5007 Å for both the central slit region (positioned at 0″) and the outer-edge slit region (positioned at 3.22″) in the left and right panels, respectively.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: Comparison of SFRs, estimated through SED fitting vs. ﹩{\mathrm{SFR}}_{\mathrm{Dn}4000}﹩ for targets in our proposal. ﹩{\mathrm{SFR}}_{\mathrm{Dn}4000}﹩ is estimated using the Dn4000 Å values from the MPA-JHU catalog (Brinchmann et al. 2004). Additionally, we compare our results with a sample of type 2 AGNs (Kim et al. 2022), estimating SFRs through SED fitting, including continuum fluxes observed at 450 and 850 μm from SCUBA-2. Offset refers to the mean difference between the values on the y-axis and the corresponding values on the x-axis, while scatter represents the standard deviation of these differences.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: Distributions of the black hole masses and bolometric luminosities of our selected sources. The sample of the proposals 2022B and 2023A semesters (M22BP038 and M23AP023) are shown in blue (L 1.4 GHz/M *  > 29.5) and red (L 1.4 GHz/M *  < 29.5) colors. Green stars show the sources of the proposal 2023B semester (M23BP013). Dashed lines indicate different Eddington ratios.
Paper: Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy
Authors: Huynh Anh N. Le, Chen Qin, Yongquan Xue, Shifu Zhu, Kim Ngan N. Nguyen, Ruisong Xia, Xiaozhi Lin
Figure caption: An integrated TPSP spectrum of J0749+4510 (z = 0.192, m r = 16.78 mag). NIR emission lines, e.g., [S III], He I, Pβ, Pα, and H2, are indicated by vertical dashed lines. The shaded regions denote areas discarded from the spectrum due to significant noise influence from sky lines or edge regions of the TPSP spectrum.
Paper: Investigation of Galactic Supernova Remnants and their Environment in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25 Using Radio Surveys
Authors: Tian-Xian Luo, Ping Zhou, Hao-Ning He
Figure caption: From top to bottom: G26.75+0.73, G27.06+0.04, G28.36+0.21, G28.78−0.44, and G29.38+0.10. Left: the THOR+VGPS continuum images of the five A17 candidates. The white circle encloses a H II that overlaps with G27.06+0.04. The magenta cross signs denote the two known pulsars spatially located within G28.36+0.21 and G29.38+0.10. The green contour shows a background radio galaxy candidate (Castelletti et al. 2017). The putative pulsar of G29.39+0.10 is marked as a yellow × sign. Middle: The four wave bands' flux density spectrum of the five A17 candidates. The blue × signs denote the flux density measured in 118 MHz, 154 MHz, and 200 MHz using GLEAM data and 1.4 GHz using THOR+VGPS continuum data, with 1-σ error bars. The red line is the best-fit line. Right: the spectral indices of the five A17 candidates between different frequency intervals derived by this work and previous works. The width of the colored bands represents the error in the spectral index. For G27.06+0.04, Dokara et al. (2018) and Dokara et al. (2021) derive the spectral index for the eastern arc. For G28.78−0.44, Dokara et al. (2021) derive the spectral index for a part of the shell.
Paper: Investigation of Galactic Supernova Remnants and their Environment in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25 Using Radio Surveys
Authors: Tian-Xian Luo, Ping Zhou, Hao-Ning He
Figure caption: The 6 σ spectral index maps overlayed with G19 SNRs (red circles), A17 SNR candidates with steep spectra (red dashed circles), the rest A17 SNR candidates (cyan circles), and the point sources that may correspond to nonthermal radiation (orange × signs) in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25. Left: the spectral index map derived from data before removing the background radiation. Right: the spectral index map derived from data after removing the background radiation and only the parts that exceed three times the average flux density of the clean region are shown to highlight the significant sources. The color bar for the spectral index is the same for both the left and right panels.
Paper: Investigation of Galactic Supernova Remnants and their Environment in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25 Using Radio Surveys
Authors: Tian-Xian Luo, Ping Zhou, Hao-Ning He
Figure caption: Top: the THOR+VGPS continuum image (red) and the 13CO (J = 1–0) 79.7 km s−1 image (cyan), overlayed with G19 SNRs (red circles), newly confirmed SNRs (red dashed circles), and the A17 SNR candidates except for the four newly confirmed SNRs (cyan circles). The molecular bubble is enclosed by a green circle. Bottom: the PV diagram along the white line in the top panel at l = 29.°1 and −1° < b < 1°.
Paper: Investigation of Galactic Supernova Remnants and their Environment in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25 Using Radio Surveys
Authors: Tian-Xian Luo, Ping Zhou, Hao-Ning He
Figure caption: THOR+VGPS 21 cm continuum data in 26.°6 < l < 30.°6, ∣b∣ ≤ 1.°25. The known SNRs in the Green’s SNR catalog (Green 2019; G19 SNRs) are enclosed by red circles, The SNR candidates discovered by Anderson et al. (2017; A17 SNR candidates) are enclosed by cyan circles, and WISE known and candidate H II regions are enclosed by white circles.