adsabs/AstroCLIMB huggingface dataset:
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: An investigation into the residual structures of the exponential-ramp method (blue) and the RECTE method (maroon). Upper panels: residuals of the exponential-ramp light curves (from Figure B1) and the RECTE light curves (from Figure B2) averaged over all visits. We combined the first seven exposures, middle six exposures, and the last six exposures of each orbit into three separate data points per orbit. Lower left: residuals of the upper panels averaged over wavelength. Lower right: averaged residual structure for an orbit. That is, to obtain the first data point, we averaged over the first data point of each orbit in the lower left panel; to obtain the second data point we averaged over the second data point of each orbit in the lower left panel; and for the third, we averaged over the third data point of each orbit. The lower level of scatter in this diagram for the exponential-ramp method shows that that method is more capable of capturing the shape of the orbit-long telescope systematics for this particular set of observations.
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: The same as Figure B1 but for the RECTE method. The residuals satisfy a Shapiro–Wilks test at the α = 0.15 level and they can thus be considered Gaussian.
Paper: An SiO Toroid and Wide-angle Outflow Associated with the Massive Protostar W75N(B)-VLA2
Authors: José F. Gómez, José M. Torrelles, Josep M. Girart, Gabriele Surcis, Jeong-Sook Kim, Jorge Cantó, Guillem Anglada, Salvador Curiel, Wouter H. T. Vlemmings, Carlos Carrasco-González, Adriana R. Rodríguez-Kamenetzky, Soon-Wook Kim, Ciriaco Goddi, Huib J. van Langevelde, Álvaro Sanchez-Monge
Figure caption: Left panel (a): Integrated intensity image (moment of order 0) of the H2CO [3(0,3)-2(0,2)] emission line in the velocity range V LSR ≃ −4 to +23 km s−1. Contour levels are 10, 20, 30, 40, 50, 60, 70, 80, and 90 percent of the maximum integrated intensity of the image, 0.54 Jy beam−1 km s−1. The synthesized beam is plotted as a yellow ellipse at the upper right corner of the image. Right panel (b): velocity field image (moment of order 1). To obtain this moment-1 image, we applied a 4σ threshold (4 mJy beam−1) to the individual spectral channels. The white line traces the half-power contour of the MOM0 image in the left panel. Ringed cross symbols for VLA1 and VLA2 indicate that these are the activity centers of strong H2O maser emission in the W75N(B) star-forming region (see, e.g., Surcis et al. 2023). The five-pointed star in both panels marks the location of the northeastern maser components in the VLA2 H2O maser shell, where the expansion appears to have halted (Surcis et al. 2023).
Paper: An SiO Toroid and Wide-angle Outflow Associated with the Massive Protostar W75N(B)-VLA2
Authors: José F. Gómez, José M. Torrelles, Josep M. Girart, Gabriele Surcis, Jeong-Sook Kim, Jorge Cantó, Guillem Anglada, Salvador Curiel, Wouter H. T. Vlemmings, Carlos Carrasco-González, Adriana R. Rodríguez-Kamenetzky, Soon-Wook Kim, Ciriaco Goddi, Huib J. van Langevelde, Álvaro Sanchez-Monge
Figure caption:                         Diagrams and image showing the various velocity components of the VLA2 SiO toroid. Upper left panel (a): position–velocity diagram of the SiO emission along the major axis of the elongated structure (PA  ≃  −53°; dashed line in Figure 4(c)) with an averaging width of 0.″14. The first contour level and the increment step are 3σ, where σ = 1.4 mJy beam−1 (the rms of the diagram). The maximum of the diagram is 44 mJy beam−1. The two “rabbit-ear-shaped” structures tracing unbound blueshifted motions are indicated. These structures originate from two peaks seen in the high-velocity blueshifted lobe (see Section 4.1 and Figure 4(c)). The dotted line indicates a possible inner velocity gradient in the SiO toroid. Upper right panel (b): same as upper left panel, but for the minor axis (PA ≃−143°; dashed line in Figure 4(c) with an averaging width of 0.″6. The first contour level is 3σ and the increment step is 6σ, where σ = 0.38 mJy beam−1. The maximum of the diagram is 32 mJy beam−1. Offset positions are with respect to the maximum SiO integrated intensity position (Figure 3(b)). Lower panel (c): integrated intensity image (moment of order 0) of the blueshifted and redshifted SiO in the high velocities ranges V                      LSR = −16.6 to −3.1 km s−1 and V                      LSR = +23.9 to +37.4 km s−1, respectively. The first contour level is 4σ and the increment step is 6σ, where σ = 5 mJy beam−1 km s−1. Symbols are as in Figure 2.
Paper: An SiO Toroid and Wide-angle Outflow Associated with the Massive Protostar W75N(B)-VLA2
Authors: José F. Gómez, José M. Torrelles, Josep M. Girart, Gabriele Surcis, Jeong-Sook Kim, Jorge Cantó, Guillem Anglada, Salvador Curiel, Wouter H. T. Vlemmings, Carlos Carrasco-González, Adriana R. Rodríguez-Kamenetzky, Soon-Wook Kim, Ciriaco Goddi, Huib J. van Langevelde, Álvaro Sanchez-Monge
Figure caption: Left panel (a): Integrated intensity image (moment of order 0) of the SiO [v = 0, 5-4] emission line in the velocity range V LSR ≃ −20 to +28 km s−1. The displayed field of view is the same as the one shown in Figure 2(a) for H2CO. Right panel (b): zoom-in showing the integrated SiO emission around VLA2. Contour levels are 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, and 0.9 Jy beam−1 km s−1. All symbols used in this figure are the same as those shown in Figure 2.
Paper: An SiO Toroid and Wide-angle Outflow Associated with the Massive Protostar W75N(B)-VLA2
Authors: José F. Gómez, José M. Torrelles, Josep M. Girart, Gabriele Surcis, Jeong-Sook Kim, Jorge Cantó, Guillem Anglada, Salvador Curiel, Wouter H. T. Vlemmings, Carlos Carrasco-González, Adriana R. Rodríguez-Kamenetzky, Soon-Wook Kim, Ciriaco Goddi, Huib J. van Langevelde, Álvaro Sanchez-Monge
Figure caption: ALMA 1.3 mm continuum emission image of the high-mass star-forming region W75N(B). The intensity range of the image has been saturated at 15 mJy beam−1 (beam = 0.″17 × 0.″08, PA = −2°; rms ≃0.08 mJy beam−1) to distinguish the faintest continuum sources, given the high dynamic range of the image (∼1100). The maximum of the image (coincident with VLA3) is 97 mJy beam−1. The position of the radio continuum sources detected in the region at centimeter wavelengths, including the massive protostars VLA1, VLA2, and VLA3, are labeled and indicated by crosses, while dotted rectangles indicate the regions MM1, MM2, and MM3 where continuum emission was previously reported at 1.3 mm with ALMA, but with a beam of 1.″73 × 0.″86, PA = −4° (Rodríguez-Kamenetzky et al. 2020). Table A1 lists the positions of all the millimeter continuum sources detected in the region (see Section 3.1, Appendix A, and Figure A1).
Paper: An SiO Toroid and Wide-angle Outflow Associated with the Massive Protostar W75N(B)-VLA2
Authors: José F. Gómez, José M. Torrelles, Josep M. Girart, Gabriele Surcis, Jeong-Sook Kim, Jorge Cantó, Guillem Anglada, Salvador Curiel, Wouter H. T. Vlemmings, Carlos Carrasco-González, Adriana R. Rodríguez-Kamenetzky, Soon-Wook Kim, Ciriaco Goddi, Huib J. van Langevelde, Álvaro Sanchez-Monge
Figure caption: Spatial distribution of the 1.3 mm continuum sources detected in a region of ∼30″ in size. Their positions (indicated here by crosses) and flux densities are listed in Table A1. The powering source of the SiO bipolar jet also detected with our ALMA observations (see Appendix C and Figure C1) is labeled as number 32 (Table A1). This source is located in between the two lobes of the SiO bipolar jet (Figure C1). The positions of the VLA continuum sources (Rodríguez-Kamenetzky et al. 2020) are also labeled and indicated by squares.
Paper: An SiO Toroid and Wide-angle Outflow Associated with the Massive Protostar W75N(B)-VLA2
Authors: José F. Gómez, José M. Torrelles, Josep M. Girart, Gabriele Surcis, Jeong-Sook Kim, Jorge Cantó, Guillem Anglada, Salvador Curiel, Wouter H. T. Vlemmings, Carlos Carrasco-González, Adriana R. Rodríguez-Kamenetzky, Soon-Wook Kim, Ciriaco Goddi, Huib J. van Langevelde, Álvaro Sanchez-Monge
Figure caption: Left panel: integrated intensity image (moment of order 0) of the SiO bipolar jet found ∼5″ northeast of VLA2 in the velocity range V LSR ≃ −3 to +43 km s−1. The position of the 1.3 mm continuum source proposed to power this SiO jet (Appendix C, Table A1) is indicated by a cross and labeled as number 32. The nearby radio continuum source VLA[NE] (Rodríguez-Kamenetzky et al. 2020) is also labeled. Other 1.3 mm continuum sources found nearby of the SiO jet are also indicated by crosses. The synthesized beam is marked as a filled yellow ellipse at the upper right corner. Right panel: velocity field image of the SiO jet (moment of order 1).
Paper: An SiO Toroid and Wide-angle Outflow Associated with the Massive Protostar W75N(B)-VLA2
Authors: José F. Gómez, José M. Torrelles, Josep M. Girart, Gabriele Surcis, Jeong-Sook Kim, Jorge Cantó, Guillem Anglada, Salvador Curiel, Wouter H. T. Vlemmings, Carlos Carrasco-González, Adriana R. Rodríguez-Kamenetzky, Soon-Wook Kim, Ciriaco Goddi, Huib J. van Langevelde, Álvaro Sanchez-Monge
Figure caption: H2CO (left panel) and SiO (right panel) lines seen in absorption toward the continuum source VLA3.
Paper: Modeling Stellar Ca II H and K Emission Variations: Spot Contribution to the S-index
Authors: K. Sowmya, A. I. Shapiro, L. H. M. Rouppe van der Voort, N. A. Krivova, S. K. Solanki
Figure caption: Panel (a): photospheric disk area coverages of faculae as a function of the corresponding spot area coverages; see the main text for details. Panel (b): S-index with spots as a function of S-index without spots. The blue curve and the gray shaded area are obtained using the spot contrast CLVs shown in Figure 3. The salmon curve represents the case where we assume that spots are as bright as the quiet star in H and K so that they are invisible in the chromosphere but are still visible as dark features in the photosphere. The black line shows the case when spots are neglected completely. Panel (c): the relationship between facular area coverages and S-index with spots (filled circles) along with the quadratic fit to this relationship (solid line). The dashed line shows the dependence of facular disk area coverage on the S-index without spots. Panel (d): the relationship between spot area coverages and S-index with spots (filled circles) along with the linear fits (cyan and black solid lines) to their relationship. The dashed line shows the dependence of spot disk area coverages on the S-index without spots.
Paper: Modeling Stellar Ca II H and K Emission Variations: Spot Contribution to the S-index
Authors: K. Sowmya, A. I. Shapiro, L. H. M. Rouppe van der Voort, N. A. Krivova, S. K. Solanki
Figure caption: Intensity images of the three sunspots scanned on 2020 August 7 at μ = 0.83 (top row), on 2021 June 22 at μ = 0.63 (middle row), and on 2022 July 7 at μ = 0.96 (bottom row). The images cover an angular area of roughly 67″ × 42″. The sunspots are shown in the continuum at ∼4001 Å (first column) and at wavelengths corresponding to H1r (second column), H2r (third column), and H3 (fourth column) as marked in Figure 2. The regions shown with lower transparency mask the areas contaminated by bright facular and plage patches. These regions are excluded from the analysis. Green boxes in each panel indicate the patches used for calculating the quiet-Sun intensity profiles shown in Figure 2. Black contours in the first column mark the boundary of the sunspot. See the main text for details.
Paper: Modeling Stellar Ca II H and K Emission Variations: Spot Contribution to the S-index
Authors: K. Sowmya, A. I. Shapiro, L. H. M. Rouppe van der Voort, N. A. Krivova, S. K. Solanki
Figure caption: CLV of the flux excess due to spots. The black circles are the SST observations (values from the fifth column of Table 1). The gray shaded region shows different scalings of the quiet-Sun CLV to match observations. The blue line is the linear fit to the observed data points. See the main text for details.
Paper: Modeling Stellar Ca II H and K Emission Variations: Spot Contribution to the S-index
Authors: K. Sowmya, A. I. Shapiro, L. H. M. Rouppe van der Voort, N. A. Krivova, S. K. Solanki
Figure caption: Average intensity profiles from the unmasked field of view in Figure 1 (maroon) and from the quiet-Sun region marked by the green box in Figure 1 (green). Intensity profiles computed using the FAL99-C model of the solar atmosphere (gray) are plotted for reference. The transmission profile of the H passband is shown by the dotted triangle. The H1r, H2r, and H3 features are also marked.
Paper: Modeling Stellar Ca II H and K Emission Variations: Spot Contribution to the S-index
Authors: K. Sowmya, A. I. Shapiro, L. H. M. Rouppe van der Voort, N. A. Krivova, S. K. Solanki
Figure caption: Panel (a): comparison between the solar S-index values computed including (maroon) and excluding (orange) the contribution from spots. Panel (b): the difference between the daily S-index values shown in panel (a) normalized to the amplitude of the solar cycle 23 in the S-index, which is 0.0149. Panel (c): 81 days smoothed values of the S-index time series plotted in panel (a). Panel (d): the difference between the 81 days averaged values shown in panel (c) normalized to the amplitude of the solar cycle 23 in the S-index.
Paper: SN 2022jli: A Type Ic Supernova with Periodic Modulation of Its Light Curve and an Unusually Long Rise
Authors: T. Moore, S. J. Smartt, M. Nicholl, S. Srivastav, H. F. Stevance, D. B. Jess, S. D. T. Grant, M. D. Fulton, L. Rhodes, S. A. Sim, R. Hirai, P. Podsiadlowski, J. P. Anderson, C. Ashall, W. Bate, R. Fender, C. P. Gutiérrez, D. A. Howell, M. E. Huber, C. Inserra, G. Leloudas, L. A. G. Monard, T. E. Müller-Bravo, B. J. Shappee, K. W. Smith, G. Terreran, J. Tonry, M. A. Tucker, D. R. Young, A. Aamer, T.-W. Chen, F. Ragosta, L. Galbany, M. Gromadzki, L. Harvey, P. Hoeflich, C. McCully, M. Newsome, E. P. Gonzalez, C. Pellegrino, P. Ramsden, M. Pérez-Torres, E. J. Ridley, X. Sheng, J. Weston
Figure caption: Top: pseudobolometric light-curve comparison of SN 2022jli and other SNe with prominent bumps and well-studied Type Ibc SNe. The bolometric light curves of the Type Ic SN 2007gr (Hunter et al. 2009), Type Ib SN 2007Y (Stritzinger et al. 2009), Type Ic iPTF15dtg (Taddia et al. 2016), Type Ib SN 2008D (Soderberg et al. 2008; Modjaz et al. 2009; pseudobolometric light curve calculated in Nicholl et al. 2015), and Type Ib/c SN 2005bf (Anupama et al. 2005) were also constructed using SUPERBOL. The dashed line represents an Arnett model (Arnett 1982) fit to the SN 2022jli light curve after MJD 59732. Bottom: MOSFiT (Guillochon et al. 2018) multiband fit results for a 56Ni explosion model (solid lines). We include the best scoring realization from a CSM + 56Ni model fit to the first 110 days of SN 2022jli as a dashed line.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Prospects for identifying neutrino emission from SNe II with CCSM in local galaxies within a distance of 2 Mpc. Here, we show the expected p-values for D * ranging from 0.01 (right edge) to 1 (left edge). The list of galaxies is complied from Nakamura et al. (2016). We present the expected p-values for IceCube (red), KM3NeT (orange hatched), joint IceCube and KM3NeT (yellow), combined IceCube, KM3NeT, and Baikal-GVD (light blue), IceCube-Gen2 (hatched blue), and combined analysis of IceCube-Gen2, KM3NeT, GVD, and P-ONE (dark blue).
Paper: SN 2022jli: A Type Ic Supernova with Periodic Modulation of Its Light Curve and an Unusually Long Rise
Authors: T. Moore, S. J. Smartt, M. Nicholl, S. Srivastav, H. F. Stevance, D. B. Jess, S. D. T. Grant, M. D. Fulton, L. Rhodes, S. A. Sim, R. Hirai, P. Podsiadlowski, J. P. Anderson, C. Ashall, W. Bate, R. Fender, C. P. Gutiérrez, D. A. Howell, M. E. Huber, C. Inserra, G. Leloudas, L. A. G. Monard, T. E. Müller-Bravo, B. J. Shappee, K. W. Smith, G. Terreran, J. Tonry, M. A. Tucker, D. R. Young, A. Aamer, T.-W. Chen, F. Ragosta, L. Galbany, M. Gromadzki, L. Harvey, P. Hoeflich, C. McCully, M. Newsome, E. P. Gonzalez, C. Pellegrino, P. Ramsden, M. Pérez-Torres, E. J. Ridley, X. Sheng, J. Weston
Figure caption: Top: GLS periodograms from BgcVroi bands, where dashed horizontal lines correspond to the 1%, 0.1%, and 0.01% FAP levels. The bottom panel shows a Lomb−Scargle periodogram generated from all bands simultaneously using gatspy. For the gr bands additional periodograms are computed using only LCO and ZTF photometry; the associated FAP levels for these periodograms are not plotted. All periodograms regardless of band or telescope−instrument combination show a significant power at ∼12.5 days. Bottom: binned phase-folded ZTF g-band and ATLAS c-band light curve. Each band has been folded on their respective best periods; the unbinned phase-folded points are shown as open symbols.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Time-integrated high-energy neutrino fluxes for neutrino emission from SNe II with CCSM at 10 kpc, for D * = 1 (red), 0.1 (blue), and 0.01 (black). The latter is the D * value that was used in Murase (2018). We show the neutrino fluences for spectral indices, s cr = 2.0 (solid) and s cr = 2.2 (dashed).
Paper: SN 2022jli: A Type Ic Supernova with Periodic Modulation of Its Light Curve and an Unusually Long Rise
Authors: T. Moore, S. J. Smartt, M. Nicholl, S. Srivastav, H. F. Stevance, D. B. Jess, S. D. T. Grant, M. D. Fulton, L. Rhodes, S. A. Sim, R. Hirai, P. Podsiadlowski, J. P. Anderson, C. Ashall, W. Bate, R. Fender, C. P. Gutiérrez, D. A. Howell, M. E. Huber, C. Inserra, G. Leloudas, L. A. G. Monard, T. E. Müller-Bravo, B. J. Shappee, K. W. Smith, G. Terreran, J. Tonry, M. A. Tucker, D. R. Young, A. Aamer, T.-W. Chen, F. Ragosta, L. Galbany, M. Gromadzki, L. Harvey, P. Hoeflich, C. McCully, M. Newsome, E. P. Gonzalez, C. Pellegrino, P. Ramsden, M. Pérez-Torres, E. J. Ridley, X. Sheng, J. Weston
Figure caption: Posterior distribution for the physical parameters of the MOSFiT default model fit to SN 2022jli. In this model f Ni is the fraction of 56Ni in the ejecta and M ej is the mass in solar masses. Ejecta velocity is V ej and ﹩\mathrm{log}\ {n}_{{\rm{H}},\mathrm{host}}﹩ is the logarithm of the host H column density. ﹩{T}_{\min }﹩ is the temperature floor as defined in Nicholl et al. (2017), and ﹩{t}_{\exp }﹩ determines the explosion epoch relative to the earliest photometry point. The σ parameter is a white-noise parameter that, when added to all data, gives a χ 2 equal to 1.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Detection probability for high-energy neutrinos from SN IIe with CCSM in IceCube and IceCube-Gen2, assuming events in the Northern sky. We show the probability of observation of at least a singlet (solid), doublet (dotted), and triplet (dashed) event for IceCube (thin) and IceCube-Gen2 (thick). Here, we consider a CR spectral index of s cr = 2.0 and the optimistic scenario (D * = 1). The blue line shows the expected CCSN rate based on Nakamura et al. (2016) with the relative fraction of SNe II with CCSM (60% of CCSNe) taken into account. See the text for details.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Detection probability for high-energy neutrinos from SN IIn in IceCube and IceCube-Gen2, assuming events in the Northern sky. We show the probability of observation of at least a singlet (solid), doublet (dotted), and triplet (dashed) event for IceCube (thin) and IceCube-Gen2 (thick). Here, we consider a CR spectral index of s cr = 2.0. The expected rate of SNe IIn is also shown with the blue band. The width of the band shows the uncertainty associated to the measured rate.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Probabilities of detecting singlet (solid), doublet (dotted), and triplet (dashed) neutrino events from SNe II with CCSM and SNe IIn up to a distance of 5 Mpc in the next generation of neutrino telescopes. Here, we consider the list of galaxies provided by Nakamura et al. (2016).
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: NIR secondary eclipse spectrum of WASP-80b measured with WFC3 (blue) and complemented with previously published Spitzer observations (black). A selection of the atmospheric models from this work are overplotted for a soot haze (upper panel), tholin haze (middle panel), and clouds (lower panel) using temperature–pressure profiles presented in Figure 3. The atmospheric models are separated into three metallicities: [M/H] = 0 (solid), [M/H] = 0.5 (dashed), and [M/H] = 1 (dotted). In each panel, we also provide the clear atmosphere models in green that are mostly thermal and only contain discernible reflective features at <0.6 μm. The best-fit models in each scenario are displayed with a bold dashed–dotted line. The best-fit tholin model tracks the clear atmosphere model very closely, as the best-fit tholin production rate is low. Diamonds denote the band-integrated eclipse depths in the WFC3/Spitzer wavelength bins for the [M/H] = 0 clear atmosphere model and for the best-fit aerosol model. It can be assumed that at ≲2.0 μm any planetary flux higher than the clear atmosphere model corresponds to light reflected by aerosols.
Paper: PSR J1953+1844 Probably Being the Descendant of an Ultracompact X-Ray Binary
Authors: Z. L. Yang, J. L. Han, W. C. Jing, W. Q. Su
Figure caption: Companion mass vs. orbital period for accreting MSPs in UCXBs and possible rotation-powered pulsar descendants. Data are taken from Guo et al. (2022), ATNF pulsar catalog (Manchester et al. 2005), and also Table 4.1 in Bhattacharyya et al. (2022). The error bars represent the mass range of these systems from ﹩\cos i=0﹩ to ﹩\cos i=0.9﹩ (90% possibility) assuming a 1.4 M ⊙ neutron star mass, with the median companion mass calculated at ﹩\cos i=0.5﹩ marked by circles and crosses for rotation-powered MSPs or accretion-powered MSPs, respectively. The binary system with a zero-temperature (zero-T) companion with a filled Roche lobe is indicated by solid curves, while that holds a companion with a zero-T radius of only one-half of the Roche lobe radius is indicated by dashed curves (Paczyński 1971; Rappaport et al. 1987). M71E is marked as a star. The parameter range roughly indicated by the two arrows is the possible long-term evolution direction in the parameter space.