adsabs/AstroCLIMB huggingface dataset:
Paper: UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation
Authors: Michael J. Koss, Ezequiel Treister, Darshan Kakkad, J. Andrew Casey-Clyde, Taiki Kawamuro, Jonathan Williams, Adi Foord, Benny Trakhtenbrot, Franz E. Bauer, George C. Privon, Claudio Ricci, Richard Mushotzky, Loreto Barcos-Munoz, Laura Blecha, Thomas Connor, Fiona Harrison, Tingting Liu, Macon Magno, Chiara M. F. Mingarelli, Francisco Muller-Sanchez, Kyuseok Oh, T. Taro Shimizu, Krista Lynne Smith, Daniel Stern, Miguel Parra Tello, C. Megan Urry
Figure caption: Left column: Keck/OSIRIS image in the J, H, and K band. Dashed circles mark the circular apertures used for 1D spectral extraction apertures (0.″3 diameter) for the northern nucleus (blue) and southern nucleus (red). Right column: spectra of the two regions (north and south), showing the bright emission lines in the region ([Fe II], warm H2, Paschen β, and Bracket γ). For the K-band spectra, we have scaled the northern source emission by a factor of 3 to enable easier comparison with the southern nucleus.
Paper: The Identification of a Dusty Multiarm Spiral Galaxy at z = 3.06 with JWST and ALMA
Authors: Yunjing Wu, Zheng Cai, Fengwu Sun, Fuyan Bian, Xiaojing Lin, Zihao Li, Mingyu Li, Franz E. Bauer, Eiichi Egami, Xiaohui Fan, Jorge González-López, Jianan Li, Feige Wang, Jinyi Yang, Shiwu Zhang, Siwei Zou
Figure caption: From left to right: reconstructed K 200-band cutout map, J 115 − K 200 color map, stellar surface density map, and lensing-corrected stellar-density/dust-continuum radial profile. Pixels belonging to A2744-DSG-z3 with fluxes higher than 2σ (determined by the pixel–pixel standard deviation) were shown. The stellar-mass surface density map is derived based on a best-fit M star/L vs. color relation. In the K 200-band map (Left panel), blue lines represent spiral arms fitted by the Logarithmic spirals equation (see Section 3.1, Equation (2)). Additionally, the ALMA dust-continuum observations are shown in the stellar surface density map (the third panel) as green contours ranging from [5, 7.5, 10] × σ. In the right panel, we obtained the effective radius of stellar mass and dust continuum from the observed radial profile, i.e., R e,star = 5.0 ± 1.5 kpc, R e,dust = 2.04 ± 0.26 kpc. Tentative foreground interloper is masked as gray lines.
Paper: The Identification of a Dusty Multiarm Spiral Galaxy at z = 3.06 with JWST and ALMA
Authors: Yunjing Wu, Zheng Cai, Fengwu Sun, Fuyan Bian, Xiaojing Lin, Zihao Li, Mingyu Li, Franz E. Bauer, Eiichi Egami, Xiaohui Fan, Jorge González-López, Jianan Li, Feige Wang, Jinyi Yang, Shiwu Zhang, Siwei Zou
Figure caption: Determinations of the redshift of DSG-z3. Left: ALMA CO (5–4) and (3–2) spectra of A2744-DSG-z3. The dashed red line shows 1σ noise spectra, while the dashed black line represents the systemic velocity. Dark-green curves show the best-fit Gaussian models of the spectra, indicating the CO-based redshift of z CO = 3.059 ± 0.001. Right: top panel shows the optimally extracted 1D spectra from NIRISS 3-band grism observations. Black histogram denotes the observed flux density, with gray shadows showing 1σ errors. The dashed red lines are the GRIZLI modeled spectra containing continuum and nebular emission templates obtained by best SED fitting. The vertical blue lines mark the location of common emission lines ([O III], Hβ, [O II], and Mg II) that are not detected in DSG-z3. The subplot at bottom right shows the probability distribution function of redshifts from SED fitting, indicating that the best grism redshift of this target is z ≈ 3.07. Bottom panels are the joint 2D spectra covered by NIRISS three filters (F115W, F150W, and F200W).
Paper: The Identification of a Dusty Multiarm Spiral Galaxy at z = 3.06 with JWST and ALMA
Authors: Yunjing Wu, Zheng Cai, Fengwu Sun, Fuyan Bian, Xiaojing Lin, Zihao Li, Mingyu Li, Franz E. Bauer, Eiichi Egami, Xiaohui Fan, Jorge González-López, Jianan Li, Feige Wang, Jinyi Yang, Shiwu Zhang, Siwei Zou
Figure caption: Top: seven-band HST observations. The red cycle indicates the location and apertures (r = 0.″5) used for this tentative foreground galaxy. Middle: photometric redshift solution based on EAZY. In the left panel, the best-fit SED is shown in blue. Meanwhile, in the right panel, the redshift probability distribution is shown in blue. The best-fit redshift (z best = 0.422) and the redshift of cluster A2744 are marked as red and orange lines, respectively. Bottom: 2D/1D JWST/NIRISS spectra of the tentative target. Each panel is the same as that in the right panel of Figure 2. We conclude that, from the grism spectra, we cannot directly determine the redshift of the tentative contamination because there are no obvious emission lines. The best-fit redshift obtain from GRIZLI is ﹩z={0.544}_{-0.003}^{+0.006}﹩. However, there is still a high-redshift solution. Thus, we cannot rule out the possibility that this target is located at the same redshift of A2744-DSG-z3.
Paper: The Identification of a Dusty Multiarm Spiral Galaxy at z = 3.06 with JWST and ALMA
Authors: Yunjing Wu, Zheng Cai, Fengwu Sun, Fuyan Bian, Xiaojing Lin, Zihao Li, Mingyu Li, Franz E. Bauer, Eiichi Egami, Xiaohui Fan, Jorge González-López, Jianan Li, Feige Wang, Jinyi Yang, Shiwu Zhang, Siwei Zou
Figure caption: Dust and stellar effective radius ratio vs. main-sequence offset (ΔMS). Blue dots are massive SFGs at z ∼ 2 reported by Tadaki et al. (2020), while the red star represents the results of A2744-DSG-z3. Shaded blue region indicates the radius ratio observed of SMGs at z ∼ 2 (Lang et al. 2019). ΔMS is defined as SFR ratios between the observed value and the expected ones on the star-forming MS. Following Aravena et al. (2020), the boundaries between passive, main-sequence, and starburst galaxies are distinguished by ΔMS = ±0.4, respectively. We conclude that, the spiral galaxy, A2744-DSG-z3, has a more compact dust core compared with SMGs at z ∼ 2 and local spirals. And the star-forming intensity is the same as main-sequence galaxies at z = 3. Our observations suggest that for A2744-DSG-z3 at z = 3, the bulge was formed with star formation at the center core region (≲2 kpc).
Paper: The Identification of a Dusty Multiarm Spiral Galaxy at z = 3.06 with JWST and ALMA
Authors: Yunjing Wu, Zheng Cai, Fengwu Sun, Fuyan Bian, Xiaojing Lin, Zihao Li, Mingyu Li, Franz E. Bauer, Eiichi Egami, Xiaohui Fan, Jorge González-López, Jianan Li, Feige Wang, Jinyi Yang, Shiwu Zhang, Siwei Zou
Figure caption: Simulated M star/L vs. color relation. Grayscale images represents the number of simulated data points with different stellar parameters (e.g., t age, Z, and A  v ). Stellar ages range from 50 Myr to 2 Gyr at z = 3.06, while metallicity ranges from 0.4 to 2.5 Z ⊙. The simulated colors are derived by adopting the Calzetti et al. (2000) law with A  V  = 0.0–2.0 (mag). Red points are median values in different color bins, while error bars are standard deviations in each bin. The blue line is a best-fit linear relation using the median points.
Paper: The Identification of a Dusty Multiarm Spiral Galaxy at z = 3.06 with JWST and ALMA
Authors: Yunjing Wu, Zheng Cai, Fengwu Sun, Fuyan Bian, Xiaojing Lin, Zihao Li, Mingyu Li, Franz E. Bauer, Eiichi Egami, Xiaohui Fan, Jorge González-López, Jianan Li, Feige Wang, Jinyi Yang, Shiwu Zhang, Siwei Zou
Figure caption: Left: JWST/NIRISS F200W observations, overlaid with contours of the CO lines (in dark red). The red cross represents the center of A2744-DSG-z3. Second to last column: CO flux density, velocity, and velocity dispersion. The synthesized beams are shown at the lower left corner of each panels with size of 1.″24 × 1.″06 (CO (5–4)) and 0.″86 × 0.″77 (CO (3–2)), respectively. The contours are drawn at [3, 4, 5] × 1σ. For mom-1 and mom-2 maps, regions with flux smaller than 2σ are masked.
Paper: Finding Peas in the Early Universe with JWST
Authors: James E. Rhoads, Isak G. B. Wold, Santosh Harish, Keunho J. Kim, John Pharo, Sangeeta Malhotra, Austen Gabrielpillai, Tianxing Jiang, Huan Yang
Figure caption: The electron temperature of [O III]-line-emitting gas is plotted as a function of the f(O III 4363)/f(O III 4959, 5007) ratio, following the treatment in Osterbrock & Ferland (2006). The solid curve shows the relation in the low-density limit, approximately n  e  < 103 cm−3. The dashed curve shows the relation for n  e  = 104 cm−3, and the dotted curve the relation for n  e  = 105 cm−3. Vertical dashed lines show the measured values of this ratio for the three z ∼ 8 galaxies. The corresponding electron temperatures are given in Table 1, and for J072326–732656 (04590) in particular exceed 30,000K in the [O III]-emitting gas. Histograms of comparison samples show that the f(O III 4363)/f(O III 4959, 5007) ratio and the electron temperature in J072326–732656 (04590) are extreme but not unprecedented in lower-redshift samples. The green histogram marks the z ≲ 0.3 Green Pea galaxy sample of Yang et al. (2019) and Jiang et al. (2019). The blue and red histograms show emission-line-selected samples at intermediate redshifts (0.2 ≲ z ≲ 0.9) from Kakazu et al. (2007) and Ly et al. (2016; with numbers multiplied by 10 and 3, respectively, to display on the same y-axis as the Green Pea sample). All comparison samples have been restricted to objects with S/N ≥ 2.5 in the [O III]4363 line.
Paper: Finding Peas in the Early Universe with JWST
Authors: James E. Rhoads, Isak G. B. Wold, Santosh Harish, Keunho J. Kim, John Pharo, Sangeeta Malhotra, Austen Gabrielpillai, Tianxing Jiang, Huan Yang
Figure caption: Blue star-shaped symbols mark the sizes and magnitudes of the JWST z ∼ 8 galaxies compared to local analogs. Left: histogram of Green Pea sizes (based on Kim et al. 2021). All three JWST sources lie in the 2nd or 3rd quartile of Green Pea sizes. Right: absolute magnitude vs. size, with contours of constant star formation intensity (i.e., orange dashed lines) marked. Gray symbols mark Green Peas. Pale blue symbols mark known Lyman continuum leakers (Izotov et al. 2016). The UV size–luminosity relation for the Green Peas, as derived in Kim et al. (2021), is plotted as a solid black line. The JWST sources are consistent with the local Green Pea relation. They populate the region of parameter space with the highest star formation intensity, which is also the region where known Lyman continuum leakers occur.
Paper: Finding Peas in the Early Universe with JWST
Authors: James E. Rhoads, Isak G. B. Wold, Santosh Harish, Keunho J. Kim, John Pharo, Sangeeta Malhotra, Austen Gabrielpillai, Tianxing Jiang, Huan Yang
Figure caption: CLOUDY model results, showing the line ratios of [O III]4363 to [O III]4959, 5007 and [O II]3726 to [O II]3729 for a grid of models with electron densities of 101.5, 102.5, and 103 cm−3 (from left to right), and gas-phase oxygen abundances ﹩12+\mathrm{log}[{\rm{O}}/{\rm{H}}]=7.5﹩, 7.1, and 6.7 (from bottom to top). Despite examining intense and low-metallicity conditions, none of the models tested reproduce the [O III]4363/[O III]4959, 5007 ratio observed in J072326–732656 (04590) (although they match the value for J072320–732604 (10612) and easily exceed that for J072322–732606 (06355), which could be matched with less extreme models). More detail on the models is presented in Section 3.3, and discussion of the implications is in Section 4.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption:  GALFIT fitting results of our sources. The two multiply imaged systems (EG-ALMA 2a/2b and EG-ALMA 6a/6b/6c) and the quasar (UDS-ALMA 2) are not included. From left to right, three panels show the original F444W (or F360M) negative image (with source name and filter noted), the fitted Sérsic model (with the index noted), and the residual (the original image with model subtracted), respectively. The images are centered on the ALMA positions and are 5″ (∼40 kpc) on a side. The depth of the TNJ1338 images is shallower than the rest, so we stacked the F300M, F335M, and F360M images to synthesize deeper broadband images with 3× longer exposure. Fitting models to the stacked images (not shown) gave sizes consistent with those from the F360M images.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: Stellar half-light radii versus stellar mass for ALMA source hosts in Figure 5. The filled symbols represent our objects, which are color coded based on their SFRs. The color bar on the right shows the coding. For comparison, the open symbols show the ultrared, flattened disks (Nelson et al. 2022), SMGs in SMACS 0723 (Cheng et al. 2022), ULIRGs in CEERS (J.-S. Huang et al. 2022 in preparation), and the SMG in A2744 (Wu et al. 2022), respectively. All values are based on NIRCam data, and we remeasured the sources in SMACS 0723 using GALFIT for consistency. The color-coded straight lines, based on the CANDELS results (Suess et al. 2019), show the relations for quiescent (lower group) and star-forming (upper group) galaxies in three redshift ranges as indicated. Most of our sources, despite the fact that they are forming stars at high rates, have sizes in the range for quiescent galaxies.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: SMG redshifts vs. 870 μm flux density. Green circles represent sources in El Gordo (with delensed flux densities), blue squares sources in UDS, and red triangles TNJ1338. For sources that do not have direct S 870 measurements (see Table 1), synthesized flux densities based on the best-fit templates from MAGPHYS are shown. Open orange diamonds show the AS2UDS sample (Stach et al. 2019), and open cyan triangles show the SUPER GOODS (Cowie et al. 2018) sample. The two multiply lensed systems, EG-ALMA 2a/2b and EG-ALMA 6a/6b/6 c, are excluded, leaving 14 targets.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: Spectrum of EG-ALMA 6 c from the ALMA 92 GHz data cube. The solid red line shows the flux-weighted central frequency of the observed emission line. If this line is CO J  =  4–3, its redshift is 4.324. This is consistent with the lensing model of Caputi et al. (2021). The dashed blue line shows where the CO J  =  4–3 line would be centered at the redshift of source ID #4a (Caputi et al. 2021).
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption:  MAGPHYS fitting results for EG-ALMA 6 c. Red circles show the NIRCam photometry (using a 0.″6 circular aperture) and the ALMA photometry. The two red arrows indicate the 3σ upper limits in the F090W and F115W bands. All values are demagnified. The black curve is the best-fitting model at the spectroscopic redshift z = 4.324. The three insets on the right are the probability density functions of the stellar mass M *, extinction A  V , and mass-weighted age. The inset on the left shows the SED near the Balmer break.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: Comparison between z phot from EAZY and MAGPHYS+PHOTOZ. Diagonal line shows equality for the two forms of z phot. For three targets (UDS-ALMA 3, UDS-ALMA 5, EG-ALMA 6a/6b/6c) with known z spec, red arrows connect the z phot to the measured z spec, indicated by red points.
Paper: JWST’s PEARLS: A JWST/NIRCam View of ALMA Sources
Authors: Cheng Cheng, Jia-Sheng Huang, Ian Smail, Haojing Yan, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Zhiyuan Ma, Anton Koekemoer, Christopher N. A. Willmer, S. P. Willner, Jose M. Diego, Brenda Frye, Christopher J. Conselice, Leonardo Ferreira, Andreea Petric, Min Yun, Hansung B. Gim, Maria del Carmen Polletta, Kenneth J. Duncan, Benne W. Holwerda, Huub J. A. Röttgering, Rachel Honor, Nimish P. Hathi, Patrick S. Kamieneski, Nathan J. Adams, Dan Coe, Tom Broadhurst, Jake Summers, Scott Tompkins, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan
Figure caption: Half-light radii vs. Sérsic indices for our SMG sample. UDS-ALMA 1/3/4/5 have compact cores, which were subtracted when calculating the half-light radii, as here we are interested only in their disk components. The SMG with n ∼ 4 is UDS-ALMA 3, which has a point source, a bar, and spiral components that skew the model fit.
Paper: Prospects for the Observation of Continuous Gravitational Waves from Spinning Neutron Stars Lensed by the Galactic Supermassive Black Hole
Authors: Soummyadip Basak, Aditya Kumar Sharma, Shasvath J. Kapadia, Parameswaran Ajith
Figure caption: Cumulative distribution of the expected number of NSs within the Einstein angle of the galactic SMBH as predicted by different models of the NS spatial distribution and galactic potential. “Progenitor” model assumes that the spatial distribution of NSs follows that of the stars in the galaxy (Paczynski 1990). Models 1A, 1B, 1C, 1D, and 1E are predicted by Sartore et al. (2010) assuming different models of NS birth velocities. The dashed curves correspond to models 1A*, 1B*, 1C*, and 1D* of Sartore et al. (2010), which assume the same NS birth velocities but a different model for the galactic potential. For the Reed et al. (2021) models, we consider different values of z 0 (shown in brackets, in kpc). The probability of at least one NS being inside the lensing cone, ﹩P({N}_{{\theta }_{E}}\geqslant 1)﹩, is ∼0.1–1, depending on the model.
Paper: Prospects for the Observation of Continuous Gravitational Waves from Spinning Neutron Stars Lensed by the Galactic Supermassive Black Hole
Authors: Soummyadip Basak, Aditya Kumar Sharma, Shasvath J. Kapadia, Parameswaran Ajith
Figure caption: Cumulative distribution of the detectable number of strongly lensed events by 3G detectors with and S/N threshold of 4.5. The probability of at least one NS being inside the lensing cone, ﹩P({N}_{{\theta }_{E}}^{\det }\geqslant 1)﹩, is ∼2%–53%, depending on the model. The gray histogram shows the results computed using a simulation using the progenitor model, while the different lines are analytical calculations using Poisson distributions.
Paper: Prospects for the Observation of Continuous Gravitational Waves from Spinning Neutron Stars Lensed by the Galactic Supermassive Black Hole
Authors: Soummyadip Basak, Aditya Kumar Sharma, Shasvath J. Kapadia, Parameswaran Ajith
Figure caption: Cumulative distribution of the S/Ns of the lensed NSs for different spatial distributions (same as Figure 2). The S/N threshold of 4.5 corresponding to a false-alarm probability of 1% and false-dismissal probability of 10% using a single-template search is shown by the vertical line.
Paper: Prospects for the Observation of Continuous Gravitational Waves from Spinning Neutron Stars Lensed by the Galactic Supermassive Black Hole
Authors: Soummyadip Basak, Aditya Kumar Sharma, Shasvath J. Kapadia, Parameswaran Ajith
Figure caption: Schematic diagram of the distribution of neutron stars (blue dots) projected onto our galactic plane. The Einstein cone of the central SMBH is shown by the gray region (highly exaggerated). The neutron stars within the Einstein cone will be strongly lensed by the SMBH.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: Overview of variations in the plume’s brightness (expressed in terms of the corrected equivalent width at a wavelength of 0.88–1.56 μm and an altitude of 85 km; see text for details) as a function of orbital phase. This figure compares the plume brightness estimates derived in this study (shown as filled circles) with previously published estimates from earlier in the Cassini mission (shown as open symbols; Hedman et al. 2013). Note that the corrected equivalent width used in this particular plot includes the phase-angle correction described in Hedman et al. (2013) in order to facilitate comparisons among the different data sets.
Paper: Establishing a Best Practice for SDTrimSP Simulations of Solar Wind Ion Sputtering
Authors: Liam S. Morrissey, Micah J. Schaible, Orenthal J. Tucker, Paul S. Szabo, Giovanni Bacon, Rosemary M. Killen, Daniel W. Savin
Figure caption: Dynamic simulations for anorthite O surface composition ratio as a function of fluence for different incidence angle cases using 1 keV H+ impacts and an O SBE of (A) 2.6 eV and (B) 6.5 eV, (C) different H+ impact energy cases using a cosine distribution of incidence angles, and (D) different SW compositions using 1 keV amu−1 impacts with a cosine distribution of incidence angles. The jaggedness of the curves is due to the Monte Carlo nature of the simulations.