adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Corner plot depicting the results of the MCMC analysis for the fitted spectrum on 2019 October 1. The histograms depict the marginalized distribution associated with each parameter. The scatter plots are overlaid with contours representing 1σ, 2σ, and 3σ levels to show the correlations between all parameters. The best-fit parameters are represented by green lines.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: (a) Different components of the continuum spectrum in the energy range of 1–3 keV at 3 MK. (b) Contribution of different elements to the free–bound continuum. The total free–bound continuum is shown in black.
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: Left: stellar mass function (SMF) for galaxies. The red symbols represent the abundance of the z ∼ 11–17 candidates in the case that they are the lower-z line-emitting red objects at z ∼ 2–5. The gray and green squares show the COSMOS2015 results for entire and quiescent galaxies (QGs) at z ∼ 3–3.5 (Davidzon et al. 2017). The green curve with the shaded region is the best-fit Schechter function with 1σ error for z ∼ 3–3.5 QGs (Davidzon et al. 2017). Right: LF for z ∼ 4–5 QSOs/AGNs compiled from the literature. The red symbols are the same as the left panel. The black line with the shaded region is the best-fit Double Power Law (DPL) function with 1σ error estimated for X-ray QSOs/AGNs (Giallongo et al. 2019). In both panels, the dashed curve represents the possible abundance of the QGs and the type II and/or dusty type I QSOs/AGNs with strong emission lines by scaling the QG SMF and the QSO/AGN LF by 4% and 40%, respectively, based on their EW([O III]+Hβ) distributions (Section 5.1), indicating that these populations can be abundant low-z interlopers in the survey volumes used for the identification of some of these z ∼ 11–17 candidates. The dotted curve in the right panel shows the 5% scaling case for reference. The M star and M UV values are taken from the best-fit SEDs forced at z < 8 with CIGALE (green curves in Figure 3). GHZ1/GLz11 in this forced lower-z solution shows M UV ∼ −10 mag, located outside of the figure in the right panel.
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: Same as Figure 3, but assuming QSO/AGN populations. The dark blue and brown dashed curves show the best-fit SED templates of type II QSO and QG+AGN populations, respectively, from the fitting range at 0 < z < 20. Both templates favor the lower-z solution (z ∼ 2–5). The Δχ 2 value in the label indicates the difference of the χ 2 value from the best-fit high-z galaxy solution shown in Figure 3. All candidates, except for GHZ1/GLz11, have the reasonable solutions at lower-z with Δχ 2 ≲ 4.
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: Fidelity of the 3D clumps as a function of S/N produced by a blind line search algorithm FINDCLUMP in our ALMA Band 7 data cube for S5-z17-1. Here we show the results with the 15 km width data cube smoothed with the six-channel kernel, where the line candidate is identified with FINDCLUMP at the 5σ level. Bottom: histograms of positive and negative clumps. Top: fidelity estimated from the histograms of positive and negative clumps as a function of S/N. The dashed line corresponds to the ∼338.7 GHz line feature exactly at the source position, indicating that the fidelity is ∼50%. Note that this is a blind search in the entire cube. Based on the survey volume only around the central target, the realistic fidelity should be much higher than 50%.
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: Best-fit MRRs for all (left) and red (right) cluster members within R 200. Colored lines illustrate how the best-fit MRRs vary as a function of the choice of richness threshold parameter, with values ranging from N th = 7 (cyan) to N th = 25 (magenta). The black (dark green) dashed line shows the MRR for the fiducial subsample of the threshold parameter in each case, i.e., ﹩{ \mathcal S }{\mathrm{all}}_{17}﹩ for all members (﹩{ \mathcal S }{\mathrm{red}}_{13}﹩ for red members) with N th = 17 (N th = 13). The upper nested panel on the left shows the scatter ﹩{f}_{\alpha 17}=({\alpha }_{{N}_{\mathrm{th}}}-{\alpha }_{{N}_{17}})/{\alpha }_{{N}_{17}}﹩ and the lower nested left shows ﹩{f}_{\beta 17}=({\beta }_{{N}_{\mathrm{th}}}-{\beta }_{{N}_{17}})/{\beta }_{{N}_{17}}﹩ relative to ﹩{\alpha }_{{N}_{17}}﹩ and ﹩{\beta }_{{N}_{17}}﹩ (black points), respectively. Nested right panels are the same as the left nested panels but relative to ﹩{\alpha }_{{N}_{13}}﹩ and ﹩{\beta }_{{N}_{13}}﹩ (green points) for N th = 13. See Appendix C for a discussion.
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: Separating red and blue members of the GalWCat19 clusters using the CMD. The left and middle panels show the CMD for cluster members in two different redshift bins. The solid cyan line in each panel shows the red-sequence ridgeline (highest probability) and the dashed line is the line that separates red and blue members at the 1σ CL from the ridgeline. The right panel shows the evolution of the ridgeline as a function redshift. The black line shows the mean color of the red members as a function of redshift with 1σ uncertainties. The nested panels show the probability distribution functions for galaxies in the CMD.
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: MRR for simulations. The mean mass at some richness bins is plotted for mini-Uchuu (left) for five v peak thresholds for subhaloes and TNG (right) for four M  s  thresholds for galaxies within r 200 as shown in each legend. Error bars represent Poisson noise. The figure shows that MRR introduces a tail at the low-richness end. The length of the tail increases with the increases in the thresholds of v peak and M  s . This indicates that the tail is dependent on the selection of the threshold and it is not intrinsic.
Paper: Nozzle Shocks, Disk Tearing, and Streamers Drive Rapid Accretion in 3D GRMHD Simulations of Warped Thin Disks
Authors: Nicholas Kaaz, Matthew T. P. Liska, Jonatan Jacquemin-Ide, Zachary L. Andalman, Gibwa Musoke, Alexander Tchekhovskoy, Oliver Porth
Figure caption: An annulus of the warped disk experiences vertical and radial oscillations twice an orbit. Panel (a): we depict the fluid frame gas density, ρ, at radius r = 13 r g and time t = 90471.8 r g/c. We have also drawn velocity streamlines of orbiting fluid parcels in black. The plot is depicted in tilted coordinates, ﹩\varphi ^{\prime} ﹩ and ﹩\theta ^{\prime} ﹩, where ﹩\varphi ^{\prime} =0﹩ indicates the local precession angle of the disk and ﹩\theta ^{\prime} =\pi /2﹩ indicates the local midplane of the disk. Panel (b): the same as the top panel, except we plot the radial mass flux ρ u  r . The radial mass flux also exhibits oscillations twice an orbit, except they are antisymmetric about the local midplane of the disk.
Paper: Nozzle Shocks, Disk Tearing, and Streamers Drive Rapid Accretion in 3D GRMHD Simulations of Warped Thin Disks
Authors: Nicholas Kaaz, Matthew T. P. Liska, Jonatan Jacquemin-Ide, Zachary L. Andalman, Gibwa Musoke, Alexander Tchekhovskoy, Oliver Porth
Figure caption: The LT torques induced by the rotation of the central BH cause the accretion disk to warp and, sometimes, tear into discrete subdisks. In each panel, we plot a 3D rendering of the fluid frame gas density, separated by δ t ≈ 1000 r g/c. Azimuthal oscillations in the scale height are apparent in the outer subdisk, where orbiting fluid parcels experience compressions and expansions twice an orbit (evidenced by the light-blue “spokes” in the outer subdisk). These oscillations are also apparent in the side-on view of the disk shown in the inset of panel (d).
Paper: The IR Compactness of Dusty Galaxies Sets Star Formation and Dust Properties at z ∼ 0–2
Authors: Jed McKinney, Alexandra Pope, Allison Kirkpatrick, Lee Armus, Tanio Díaz-Santos, Carlos Gómez-Guijarro, Maximilien Franco, David Elbaz, Christopher C. Hayward, Hanae Inami, Gergö Popping, Mengyuan Xiao
Figure caption: The effective IR size as a function of total IR luminosity powered by star formation. Galaxies in our ALMA-detected sample are shown with symbols corresponding to their f AGN,MIR classification. We compare against the archival sample of Fujimoto et al. (2017; black 16%, 50%, 84% contours), GOALS (purple circles) and KINGFISH (gray diamonds). We have subtracted out the contribution to L IR from AGNs in our sample and GOALS using f AGN,MIR and Equation (5) from Kirkpatrick et al. (2015). Dashed lines correspond to constant SFR surface densities. The shaded gray region indicates ΣSFR > 1000 M ⊙ yr−1 where star formation exceeds the Eddington limit (Andrews & Thompson 2011). Normalized histograms of R eff for each sample are plotted along the right y-axis. (U)LIRGs have ΣSFR ∼ 1−100 M ⊙ yr−1, with z ∼ 2 galaxies from this work having higher L IR,SF and greater R eff than the average at z ∼ 0. The three z ∼ 2 composite galaxies close to ΣSFR ∼ 1000 M ⊙ yr−1 are all above the main sequence for their stellar mass and SFR.
Paper: The IR Compactness of Dusty Galaxies Sets Star Formation and Dust Properties at z ∼ 0–2
Authors: Jed McKinney, Alexandra Pope, Allison Kirkpatrick, Lee Armus, Tanio Díaz-Santos, Carlos Gómez-Guijarro, Maximilien Franco, David Elbaz, Christopher C. Hayward, Hanae Inami, Gergö Popping, Mengyuan Xiao
Figure caption: The ratio of the 6.2 μm PAH luminosity relative to the total dust mass in our z ∼ 2 ALMA-detected Spitzer/IRS sample (blue, following the AGN classification symbols of Figure 1), GOALS (pink circles), and KINGFISH (gray diamonds) as a function of ΣIR,SF. A histogram showing the distribution in L PAH(6.2 μm)/M dust for each sample is shown along the right. The scatter in L PAH(6.2 μm)/M dust is marginally larger for z > 0 relative to GOALS, owing to the lower S/N mid-IR spectra and larger error bars. Nevertheless, both (U)LIRG samples cluster around an average ﹩\mathrm{log}\,{{\rm{L}}}_{\mathrm{PAH}(6.2\,\mu {\rm{m}})}/{{\rm{M}}}_{\mathrm{dust}}﹩ ∼1.3 ± 0.4 L ⊙/M ⊙, as shown with the shaded region in the left panel, with no clear correlation against ΣIR,SF. KINGFISH galaxies, on the other hand, do show a positive correlation between L PAH(6.2 μm)/M dust and ΣIR,SF (solid red line) with small 1σ dispersion about the best-fit (dashed red line), but the overall range is consistent with ratios found among (U)LIRGs.
Paper: The IR Compactness of Dusty Galaxies Sets Star Formation and Dust Properties at z ∼ 0–2
Authors: Jed McKinney, Alexandra Pope, Allison Kirkpatrick, Lee Armus, Tanio Díaz-Santos, Carlos Gómez-Guijarro, Maximilien Franco, David Elbaz, Christopher C. Hayward, Hanae Inami, Gergö Popping, Mengyuan Xiao
Figure caption: A comparison between the effective IR size and the total dust mass for (U)LIRGs at z ∼ 2 (blue symbols, following f AGN,MIR classifications in Figure 4), GOALS (pink circles), and KINGFISH (gray diamonds). Grey dashed lines correspond to constant levels of gas mass surface densities assuming a dust-to-gas ratio of 0.01. The shaded regions represent the 16th–84th percentile distribution in dust-continuum size vs. dust mass from galaxies in the TNG50 cosmological simulation at z ∼ 1–2 (Popping et al. 2022). Dotted–dashed lines of the corresponding color represent TNG50 galaxies 2σ below the median. Luminous IR galaxies at z ∼ 2 tend to have higher dust masses and be more extended than their local counterparts in GOALS, except for the three most luminous starbursts in our sample that all have 25% < f AGN,MIR < 40% and have star formation rates >3× greater than main-sequence galaxies for their redshifts and stellar masses. The sizes we measure at z ∼ 2 and those in (U)LIRGs at z = 0 are consistent with the more compact (lower R eff) galaxies in TNG50 for fixed dust mass (dashed/dashed–dotted lines), and have Σgas ∼ 103 M ⊙ pc−2.
Paper: The IR Compactness of Dusty Galaxies Sets Star Formation and Dust Properties at z ∼ 0–2
Authors: Jed McKinney, Alexandra Pope, Allison Kirkpatrick, Lee Armus, Tanio Díaz-Santos, Carlos Gómez-Guijarro, Maximilien Franco, David Elbaz, Christopher C. Hayward, Hanae Inami, Gergö Popping, Mengyuan Xiao
Figure caption: Top: distribution in L IR among galaxies matched to ALMA archival detections (blue) compared against nondetections within the footprint of an archival observation (brown) and the parent GOODS-S sample (gray). Colored squares and their errors show the mean and standard deviation of the corresponding distribution. Our catalog of ALMA-detected sources spans the range in L IR of the parent sample, but is biased high, on average, by ∼0.2 dex. Bottom: integrated ALMA flux vs. L IR for detections and nondetections. Different symbols correspond to the mid-IR AGN classifications as labeled in the caption. Upper limits generally cluster around ∼0.3 mJy as most fall within the ASAGAO footprint (Fujimoto et al. 2018; Ueda et al. 2018). Note that the four ∼10 mJy sources are detected with Band 9 at λ obs ∼ 450 μm compared to ∼1.2 μm for the rest of the sample. A 25 K blackbody is ∼10× more luminous at 450 μm than at 1.2 mm, which is approximately the difference in flux between our Band 9 and Band 6 archival detections.
Paper: The IR Compactness of Dusty Galaxies Sets Star Formation and Dust Properties at z ∼ 0–2
Authors: Jed McKinney, Alexandra Pope, Allison Kirkpatrick, Lee Armus, Tanio Díaz-Santos, Carlos Gómez-Guijarro, Maximilien Franco, David Elbaz, Christopher C. Hayward, Hanae Inami, Gergö Popping, Mengyuan Xiao
Figure caption: The ratio of total IR luminosity to total dust mass as a function of IR size in z ∼ 0–2 (U)LIRGs (GOALS, this work) and KINGFISH galaxies at lower SFR surface densities. The legend follows Figures 4 and 5. Smaller galaxies in KINGFISH tend to have larger L IR,SF/M dust and eventually fall within the scatter of z ∼ 0–2 (U)LIRGs with low L IR/M dust by R eff  ∼ 1−2 kpc. The anticorrelation between L IR,SF/M dust and R eff at z ∼ 0 including (U)LIRGs and more normal star-forming galaxies is strong (r  p , p) = (−0.65, 10−15). (U)LIRGs at z ∼ 2 do not exhibit such an anticorrelation, but have comparable L IR/M dust to local (U)LIRGs, albeit at higher R eff on average.
Paper: Pulsar Timing Array Detections of Supermassive Binary Black Holes: Implications from the Detected Common Process Signal and Beyond
Authors: Yunfeng Chen, Qingjuan Yu, Youjun Lu
Figure caption: Distributions of the individual BBHs that are detectable by the two CPTA configurations (left) and by the two SKAPTA configurations (right), in the source parameter space of the total mass M BH, mass ratio q BH, redshift z, and detection S/N ρ. In both panels, the ﹩{delay}-{{ \mathcal A }}_{\max }^{{\rm{e}}}﹩ model is adopted. The blue and red colors correspond to the optimistic PTA configurations and the conservative PTA configurations, respectively. As for the optimistic PTA configurations, the detectable sources from 10 realizations of the global BBH population are shown, and for the conservative PTA configurations, the detectable sources from 10,000 realizations of the global BBH population are shown. The one-dimensional histograms in the top panels show the number distributions of the detectable sources. This figure shows that the small sample of the BBHs detected at the beginning tends to have larger masses (peaking at ∼4 × 109 M ⊙), larger mass ratios (close to 1), and lower redshifts (∼0.1), compared with the large BBH populations to be detected by the optimistic PTAs. See Section 4.2.2 for details.
Paper: Pulsar Timing Array Detections of Supermassive Binary Black Holes: Implications from the Detected Common Process Signal and Beyond
Authors: Yunfeng Chen, Qingjuan Yu, Youjun Lu
Figure caption: Distributions of the individual BBHs that are detectable by the optimistic-CPTA (left) and the optimistic-SKAPTA (right), in the source parameter space of the total mass M BH, mass ratio q BH, redshift z, and detection S/N ρ. The red and blue colors in the figure correspond to the delay-﹩{{ \mathcal A }}_{1}﹩ and delay-﹩{{ \mathcal A }}_{1}^{z}﹩ models, respectively. For both models, the sources from one single realization of the global BBH population are shown in the figure. The one-dimensional histograms in the top panels show the number distributions of the detectable sources. This figure shows that the different models, i.e., with and without redshift evolution, result in different redshift distributions of the detectable BBHs (e.g., different peak heights and relative number ratios of low-z to high-z sources). See Section 4.2.2 for details.
Paper: The IR Compactness of Dusty Galaxies Sets Star Formation and Dust Properties at z ∼ 0–2
Authors: Jed McKinney, Alexandra Pope, Allison Kirkpatrick, Lee Armus, Tanio Díaz-Santos, Carlos Gómez-Guijarro, Maximilien Franco, David Elbaz, Christopher C. Hayward, Hanae Inami, Gergö Popping, Mengyuan Xiao
Figure caption: Distribution in specific star formation rates (sSFR  ≡ SFR/M*) relative to the main sequence (ΔsSFMS): the difference between each galaxy’s sSFR and the corresponding main-sequence sSFR for its stellar mass and redshift. We adopt the main-sequence parameterization of Speagle et al. (2014). The color scheme follows the top panel of Figure 1. The ALMA-detected sources have ΔsSFMS distributed similarly to undetected archival targets, and consist of five galaxies below common thresholds used to identify starbursts (dashed black line; Puglisi et al. 2021) and 10 galaxies above.
Paper: TESS Photometric Variability of Young Brown Dwarfs in the Taurus Star-forming Region
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram
Figure caption: The light curves of all selected BDs in the Taurus star-forming region are shown here. The left column showcases the complete light curves, displayed in black, while the binned light curves with a binning interval of 500 minutes are depicted as red dots. In the middle column, the LS periodograms are showcased, illustrating the power spectra of the BDs’ rotational periods. Finally, the right column displays the phase-folded light curves, where the data are folded with the most significant peak obtained from the LS periodogram. The black stars represent the 1000-point binned data. The object names, TIC IDs, and sectors are included in the figure titles in the left column. Additionally, the rotation periods of the BDs are mentioned within the phase light curves.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: The S/N for various detectors as a function of integration time for a poloidal magnetic field–dominated NS with initial ν = 100 Hz, χ = 3°, B  P  = 1015 G (L  D  > L GW;  top panel) and B  P  = 1012 G (L GW > L  D ;  bottom panel) for two cases from Table 6. The orange line corresponds to <S/N > = 12.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: The S/N for various detectors as a function of integration time for a toroidal magnetic field–dominated NS with initial χ = 3°, initial ν = 500 Hz, ﹩{B}_{\max }=1.4\times {10}^{17}﹩ G (top panel), and ﹩{B}_{\max }=9\times {10}^{16}﹩ G (bottom panel) for two cases from Table 7. The orange line corresponds to 〈S/N〉 = 12.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: The S/N for various detectors as a function of integration time for a toroidal magnetic field–dominated NS with initial χ = 3°, ﹩{B}_{\max }=9\times {10}^{16}﹩ G, initial ν = 500 Hz (top panel), and ν = 200 Hz (bottom panel) for two cases from Table 7. The orange line corresponds to 〈S/N〉 = 12.
Paper: TESS Photometric Variability of Young Brown Dwarfs in the Taurus Star-forming Region
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram
Figure caption: The left panel shows the PDCSAP light curve (red) and the detrended light curve (blue) of MHO 4 in TESS sector 43. The right panel shows the zoomed-in view of the flare. The x-axis corresponds to the time in Barycentric TESS Julian Days (BTJD), and the y-axis corresponds to the TESS flux (e −1/s).