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Full list of authors: De Marco, Orsola; Akashi, Muhammad; Akras, Stavros; Alcolea, Javier; Aleman, Isabel; Amram, Philippe; Balick, Bruce; De Beck, Elvire; Blackman, Eric G.; Boffin, Henri M. J.; Boumis, Panos; Bublitz, Jesse; Bucciarelli, Beatrice; Bujarrabal, Valentin; Cami, Jan; Chornay, Nicholas; Chu, You-Hua; Corradi, Romano L. M.; Frank, Adam; García-Hernández, D. A.; García-Rojas, Jorge; García-Segura, Guillermo; Gómez-Llanos, Veronica; Gonçalves, Denise R.; Guerrero, Martín A.; Jones, David; Karakas, Amanda I.; Kastner, Joel H.; Kwok, Sun; Lykou, Foteini; Manchado, Arturo; Matsuura, Mikako; McDonald, Iain; Miszalski, Brent; Mohamed, Shazrene S.; Monreal-Ibero, Ana; Monteiro, Hektor; Montez, Rodolfo; Baez, Paula Moraga; Morisset, Christophe; Nordhaus, Jason; Mendes de Oliveira, Claudia; Osborn, Zara; Otsuka, Masaaki; Parker, Quentin A.; Peeters, Els; Quint, Bruno C.; Quintana-Lacaci, Guillermo; Redman, Matt; Ruiter, Ashley J.; Sabin, Laurence; Sahai, Raghvendra; Contreras, Carmen Sánchez; Santander-García, Miguel; Seitenzahl, Ivo; Soker, Noam; Speck, Angela K.; Stanghellini, Letizia; Steffen, Wolfgang; Toalá, Jesús A.; Ueta, Toshiya; Van de Steene, Griet; Van Winckel, Hans; Ventura, Paolo; Villaver, Eva; Vlemmings, Wouter; Walsh, Jeremy R.; Wesson, Roger; Zijlstra, Albert A., Planetary nebulae—the ejected envelopes of red giant stars—provide us with a history of the last, mass-losing phases of 90% of stars initially more massive than the Sun. Here we analyse images of the planetary nebula NGC 3132 from the James Webb Space Telescope (JWST) Early Release Observations. A structured, extended hydrogen halo surrounding an ionized central bubble is imprinted with spiral structures, probably shaped by a low-mass companion orbiting the central star at about 40–60 au. The images also reveal a mid-infrared excess at the central star, interpreted as a dusty disk, which is indicative of an interaction with another closer companion. Including the previously known A-type visual companion, the progenitor of the NGC 3132 planetary nebula must have been at least a stellar quartet. The JWST images allow us to generate a model of the illumination, ionization and hydrodynamics of the molecular halo, demonstrating the power of JWST to investigate complex stellar outflows. Furthermore, new measurements of the A-type visual companion allow us to derive the value for the mass of the progenitor of a central star with excellent precision: 2.86 ± 0.06 M⊙. These results serve as pathfinders for future JWST observations of planetary nebulae, providing unique insight into fundamental astrophysical processes including colliding winds and binary star interactions, with implications for supernovae and gravitational-wave systems. © 2022, The Author(s), under exclusive licence to Springer Nature Limited., We acknowledge the International Astronomical Union that oversees the work of Commission H3 on Planetary Nebulae. It is through the coordinating activity of this committee that this paper came together. S.A. acknowledges support under the grant 5077 financed by IAASARS/NOA. J.A. and V.B. acknowledge support from the EVENTs/Nebulae-Web research programme, Spanish AEI grant PID2019-105203GB-C21. I.A. acknowledges the support of CAPES, Brazil (Finance Code 001). E.D.B. acknowledges financial support from the Swedish National Space Agency. E.G.B. acknowledges NSF grants AST-1813298 and PHY-2020249. J.C. and E.P. acknowledge support from an NSERC Discovery Grant. G.G.-S. thanks M. L. Norman and the Laboratory for Computational Astrophysics for the use of ZEUS-3D. D.A.G.-H. and A.M. acknowledge support from the ACIISI, Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant with reference PROID2020010051 as well as from the State Research Agency (AEI) of the Spanish Ministry of Science and Innovation (MICINN) under grant PID2020-115758GB-I00. J.G.-R. acknowledges support from Spanish AEI under Severo Ochoa Centres of Excellence Programme 2020-2023 (CEX2019-000920-S). J.G.-R. and V.G.-L. acknowledge support from ACIISI and ERDF under grant ProID2021010074. D.R.G. acknowledges the CNPq grant 313016/2020-8. M.A.G. acknowledges support of grant PGC2018-102184-B-I00 of the Ministerio de Educación, Innovación y Universidades cofunded with FEDER funds and from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). D.J. acknowledges support from the Erasmus+ programme of the European Union under grant number 2020-1-CZ01-KA203-078200. A.I.K. and Z.O. were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research is/was supported by an Australian Government Research Training Program (RTP) Scholarship. M.M. and R.W. acknowledge support from STFC Consolidated grant (2422911). C.M. acknowledges support from UNAM/DGAPA/PAPIIT under grant IN101220. S.S.M. acknowledges funding from UMiami, the South African National Research Foundation and the University of Cape Town VC2030 Future Leaders Award. J.N. acknowledges support from NSF grant AST-2009713. C.M.d.O. acknowledges funding from FAPESP through projects 2017/50277-0, 2019/11910-4 e 2019/26492-3 and CNPq, process number 309209/2019-6. J.H.K. and P.M.B. acknowledge support from NSF grant AST-2206033 and a NRAO Student Observing Support grant to Rochester Institute of Technology. M.O. was supported by JSPS Grants-in-Aid for Scientific Research(C) (JP19K03914 and 22K03675). Q.A.P. acknowledges support from the HKSAR Research grants council. Vera C. Rubin Observatory is a Federal project jointly funded by the National Science Foundation (NSF) and the Department of Energy (DOE) Office of Science, with early construction funding received from private donations through the LSST Corporation. The NSF-funded LSST (now Rubin Observatory) Project Office for construction was established as an operating centre under the management of the Association of Universities for Research in Astronomy (AURA). The DOE-funded effort to build the Rubin Observatory LSST Camera (LSSTCam) is managed by SLAC National Accelerator Laboratory (SLAC). A.J.R. was supported by the Australian Research Council through award number FT170100243. L.S. acknowledges support from PAPIIT UNAM grant IN110122. C.S.C.’s work is part of I+D+i project PID2019-105203GB-C22 funded by the Spanish MCIN/AEI/10.13039/501100011033. M.S.-G. acknowledges support by the Spanish Ministry of Science and Innovation (MICINN) through projects AxIN (grant AYA2016-78994-P) and EVENTs/Nebulae-Web (grant PID2019-105203GB-C21). R.S.’s contribution to the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. J.A.T. thanks the Marcos Moshisnky Fundation (Mexico) and UNAM PAPIIT project IA101622. E.V. acknowledges support from the ‘On the rocks II project’ funded by the Spanish Ministerio de Ciencia, Innovación y Universidades under grant PGC2018-101950-B-I00. A.A.Z. acknowledges support from STFC under grant ST/T000414/1. This research made use of Photutils, an Astropy package for detection and photometry of astronomical sources83, of the Spanish Virtual Observatory (https://svo.cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00 and of the computing facilities available at the Laboratory of Computational Astrophysics of the Universidade Federal de Itajubá (LAC-UNIFEI, which is maintained with grants from CAPES, CNPq and FAPEMIG).

We report observations and modeling of the stellar remnant and presumed double-degenerate merger of Type~Iax supernova Pa30, which is the probable remnant of SN~1181~AD. It is the only known bound stellar SN remnant and the only star with Wolf-Rayet features that is neither a planetary nebula central star nor a massive Pop I progenitor. We model the unique emission-line spectrum with broad, strong O~{\sc vi} and O~{\sc viii} lines as a fast stellar wind and shocked, hot gas. Non-LTE wind modeling indicates a mass-loss rate of $\sim 10^{-6}\,\rm M_\odot\,yr^{-1}$ and a terminal velocity of $ \sim$15,000~km\,s$^{-1}$, consistent with earlier results. O~{\sc viii} lines indicate shocked gas temperatures of $T \simeq 4\,$MK. We derive a magnetic field upper limit of $B, 20 pages, 13 figures, 3 tables. Matches version accepted for publication by ApJ

e present the first 3D radiation-hydrodynamic simulations on the formation and evolution of born-again planetary nebulae (PNe), with particular emphasis to the case of HuBi 1, the inside-out PN. We use the extensively tested GUACHO code to simulate the formation of HuBi 1 adopting mass-loss and stellar wind terminal velocity estimates obtained from observations presented by our group. We found that, if the inner shell of HuBi 1 was formed by an explosive very late thermal pulse (VLTP) ejecting material with velocities of ∼300 km s−1, the age of this structure is consistent with that of ≃200 yr derived from multi-epoch narrow-band imaging. Our simulations predict that, as a consequence of the dramatic reduction of the stellar wind velocity and photon ionizing flux during the VLTP, the velocity and pressure structure of the outer H-rich nebula are affected creating turbulent ionized structures surrounding the inner shell. These are indeed detected in Gran Telescopio Canarias MEGARA optical observations. Furthermore, we demonstrate that the current relatively low ionizing photon flux from the central star of HuBi 1 is not able to completely ionize the inner shell, which favours previous suggestions that its excitation is dominated by shocks. Our simulations suggest that the kinetic energy of the H-poor ejecta of HuBi 1 is at least 30 times that of the clumps and filaments in the evolved born-again PNe A 30 and A 78, making it a truly unique VLTP event. © 2021 The Author(s)., JAT thanks funding by Fundación Marcos Moshinsky (Mexico) and the Direcciónn General de Asuntos del Personal Académico (DGAPA) of the Universidad Nacional Autónoma de México (UNAM) project IA100720. VL gratefully acknowledges support from the CONACYT Research Fellowship program. BMM and MAG acknowledge support of the Spanish Ministerio de Ciencia, Innovación y Universidades (MCIU) grant PGC2018-102184-B-I00. AE acknowledges support from DGAPA-PAPIIT (UNAM) grant IN 109518. This work has made extensive use of NASA’s Astrophysics Data System., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

We present an infrared (IR) characterization of the born-again planetary nebulae (PNe) A 30 and A 78 using IR images and spectra. We demonstrate that the carbon-rich dust in A 30 and A 78 is spatially coincident with the H-poor ejecta and coexists with hot X-ray-emitting gas up to distances of 50 arcsec from the central stars of PNe (CSPNe). Dust forms immediately after the born-again event and survives for 1000 yr in the harsh environment around the CSPN as it is destroyed and pushed away by radiation pressure and dragged by hydrodynamical effects. Spitzer IRS spectral maps showed that the broad spectral features at 6.4 and 8.0 μm, attributed to amorphous carbon formed in H-deficient environments, are associated with the disrupted disc around their CSPN, providing an optimal environment for charge exchange reactions with the stellar wind that produces the soft X-ray emission of these sources. Nebular and dust properties are modelled for A 30 with cloudy taking into account different carbonaceous dust species. Our models predict dust temperatures in the 40-230 K range, five times lower than predicted by previous works. Gas and dust masses for the born-again ejecta in A 30 are estimated to be Mgas=4.41+0.550.14× 10-3 M· and M dust=3.20+3.21-2.06× 10-3 M·, which can be used to estimate a total ejected mass and mass-loss rate for the born-again event of 7.61+3.76-2.20× 10-3 M· and M=(5-60)× 10-5 M· yr-1, respectively. Taking into account the carbon trapped into dust grains, we estimate that the C/O mass ratio of the H-poor ejecta of A 30 is larger than 1, which favours the very late thermal pulse model over the alternate hypothesis of a nova-like event. © 2021 The Author(s)., The authors acknowledge funding by Direccion General de Asuntos del Personal Academico of the Universidad Nacional Autonoma de Mexico (DGAPA, UNAM) project IA100720. JAT thanks Fundacion Marcos Moshinsky (Mexico). VMAGG acknowledges support from the Programa de Becas posdoctorales funded by DGAPA, UNAM. JBRG, SED, and PJH thank Consejo Nacional deCiencias yTecnolog ' ia(CONACYT) Mexico for research student grants. MAGacknowledges support of the SpanishMinisterio de Ciencia, Innovacion y Universidades (MCIU) grant PGC2018-102184-B-I00. GRL acknowledges support from CONACYT (grant 263373) and PRODEP (Mexico). DAGH acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant AYA2017-88254-P. This study is based on observations made with the instruments NOTCam at the Nordic Optical Telescope (NOT) and CanariCam at the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. NOT is owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku, and the University of Oslo, representing Denmark, Finland, and Norway, the University of Iceland, and Stockholm University. This work makes use of Spitzer IR observations, which was operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is partially based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work has made extensive use of NASA's Astrophysics Data System., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., Born-again planetary nebulae (PNs) allow investigating stellar evolution, dust production, and nebular shocks in human timescales. Here we present an analysis of multiepoch optical spectroscopic observations of the born-again PN A 58 around V605 Aql, which experienced a very late thermal pulse about a century ago. The H-deficient ejecta has experienced a considerable brightening in the time period considered, from 1996 to 2021, with notable changes also in many emission line ratios. Neither the reduction of the extinction caused by the dilution of the ejecta nor the increase of the ionizing photon flux from the central star seem capable to produce these spectral changes, which are instead attributed to shocks in the bipolar H-poor outflow, dissociating molecular material, and propagating through the outer nebula. © 2022. The Author(s). Published by the American Astronomical Society., B.M.M. and M.A.G. are funded by the Spanish Ministerio de Ciencia, Innovación y Universidades (MCIU) grant PGC2018-102184-B-I00, co-funded by FEDER funds. B.M.M. and M.A.G. acknowledge support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa' award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). J.A.T. thanks funding by Fundación Marcos Moshinsky (Mexico) and the DGAPA UNAM project IA101622. J.B.R.G. acknowledges Consejo Nacional de Ciencia y Tecnología (CONACyT, Mexico) for a student scholarship. The authors thank D. Tafoya for fruitful discussion during the preparation of the manuscript. We also thank H. Todt for providing us with the stellar atmosphere model of V 605 Aql. This work made use of IRAF, distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the National Science Foundation. This work has made extensive use of NASA's Astrophysics Data System.

We present the analysis of archival Very Large Telescope (VLT) Multi-Unit Spectroscopic Explorer (MUSE) observations of the interacting galaxies NGC 4038/39 (a.k.a. the Antennae) at a distance of 18.1 Mpc. Up to 38 young star-forming complexes with evident contribution from Wolf-Rayet (WR) stars are unveiled. We use publicly available templates of Galactic WR stars in conjunction with available photometric extinction measurements to quantify and classify the WR population in each star-forming region, on the basis of its nearly Solar oxygen abundance. The total estimated number of WR stars in the Antennae is 4053 ± 84, of which there are 2021 ± 60 WNL and 2032 ± 59 WC-types. Our analysis suggests a global WC to WN-type ratio of 1.01 ± 0.04, which is consistent with the predictions of the single star evolutionary scenario in the most recent bpass stellar population synthesis models. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society., The authors thank the referee for valuable suggestions that clarified our estimations on the number of WR stars in the Antennae. VMAGG acknowledges support from the Programa de Becas posdoctorales funded by Direccion General de Asuntos del Personal Academico (DGAPA) of the Universidad Nacional Autonoma de Mexico (UNAM). VMAGG thanks Nate Bastian for kindly sharing his WR spectra for a preliminary analysis that prompted the interest in this study. The authors are thankful to JJ Eldridge for kindly sharing their models to compare with our results. VMAGG, JAT, and SJA acknowledge funding by DGAPA UNAM PAPIIT projects IA100720 and IN107019. This work is based on data obtained from the ESO Science Archive Facility, program ID: 095.B-0042, and observations from GTC public data base. Observations made with theNASA/ESA Hubble Space Telescope were obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology.

We present a comprehensive infrared (IR) study of the iconicWolf-Rayet (WR) wind-blown bubble NGC6888 around WR136. We use Wide-field Infrared Survey Explorer, Spitzer IRAC, and MIPS and Herschel PACS IR images to produce a sharp view of the distribution of dust around WR136. We complement these IR photometric observations with Spitzer IRS spectra in the 5-38-mu m wavelength range. The unprecedented high-resolution IR images allowed us to produce a clean spectral energy distribution, free of contamination from material along the line of sight, to model the properties of the dust in NGC6888. We use the spectral synthesis code CLOUDY to produce a model for NGC6888 that consistently reproduces its optical and IR properties. Our best model requires a double distribution with the inner shell composed only of gas, whilst the outer shell requires a mix of gas and dust. The dust consists of two populations of grain sizes, one with small-sized grains a(small) = [0.002-0.008] mu m and another one with large-sized grains a(big) = [0.05-0.5] mu m. The population of big grains is similar to that reported for other red supergiants stars and dominates the total dust mass, which leads us to suggest that the current mass of NGC6888 is purely due to material ejected from WR 136, with a negligible contribution of the swept up interstellar medium. The total mass of this model is 25.5(-2.8)+4.7 M-circle dot, a dust mass of M-dust = 0.14(-0.01)(+0.03) M circle dot, for a dust-to-gas ratio of 5.6 x 10(-3). Accordingly, we suggest that the initial stellar mass of WR 136 was less than or similar to 50 M-circle dot, consistent with current single stellar evolution models. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society, The authors are also thankful to J. Reyes-Perez for providing the CMFGEN model of WR 136. GR would like to thank S.J. Arthur and people at IRyA-UNAM for their support during the realization of this project. GR, ES and JAQ-M acknowledge support from Consejo Nacional de Ciencia y Tecnologia (CONACyT) for student scholarship. JAT, GR, and MAG are funded by UNAM DGAPA PAPIIT project IA100720. MAG acknowledges support of the Spanish Ministerio de Ciencia, Innovaci ' on y Universidades grant PGC2018-102184-B-I00, co-funded by FEDER funds. GR-L acknowledges support from CONACyT grant 263373 and PRODEP (Mexico). VMAGG acknowledges support from the Programa de Becas posdoctorales of DGAPA UNAM. This work makes use of IRAF, distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the National Science Foundation. This work makes use of Herschel, Spitzer, and WISE IR observations. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The Spitzer Space Telescope was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by < 0:funding-source 3:href="http://dx.doi.org/10.13039/100000104"> NASA through an award issued by JPL/Caltech. WISE is a joint project of the University of California (Los Angeles, USA) and the JPL/Caltech, funded by < 0:funding-sourc e 3:href="http://dx.doi.org/10.13039/100000104"> NASA .

The Advanced CCD Imaging Spectrometer (ACIS-S) camera on board the Chandra X-ray Observatory has been used to discover a hot bubble in the planetary nebula (PN) IC 4593, the most distant PN detected by Chandra so far. The data are used to study the distribution of the X-ray-emitting gas in IC 4593 and to estimate its physical properties. The hot bubble has a radius of similar to 2 arcsec and is found to be confined inside the optically bright innermost cavity of IC 4593. The X-ray emission is mostly consistent with that of an optically thin plasma with temperature kT approximate to 0.15 keV (or T-X approximate to 1.7 x 10(6) K), electron density n(e) approximate to 15 cm(-3) , and intrinsic X-ray luminosity in the 0.3-1.5 keV energy range L-X = 3.4 x 10(30) erg s(-1). A careful analysis of the distribution of hard (E >0.8 keV) photons in IC4593 suggests the presence of X-ray emission from a point source likely associated with its central star (CSPN). If this was the case, its estimated X-ray luminosity would be L-X,(CSPN) = 7 x 10(29) erg s(-1), fulfilling the log(L-X, (CSPN)/L-bol) approximate to -7 relation for self-shocking winds in hot stars. The X-ray detection of the CSPN helps explain the presence of high-ionization species detected in the ultraviolet spectra as predicted by stellar atmosphere models. © 2020 The Author(s)., JAT and MAG are supported by the Universidad Nacional Autonoma de Mexico (UNAM) Direccion General de Asuntos del Personal Academico (DGAPA) PAPIIT projects IA100318 and IA100720. MAG acknowledges support from grant PGC2018102184-B-I00, co-funded with FEDER funds. LB and YHC acknowledge support from NASA grant Chandra GO2-13024B. YHC acknowledges the research grant 108-2112-M-001-045 from the Ministry of Science and Technology (MOST) of Taiwan. This work has made extensive use of the NASA's Astrophysics Data System. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We present the analysis of archival XMM-Newton European Photon Imaging Camera (EPIC) X-ray observations of the symbiotic star R Aquarii. We used the Extended Source Analysis Software package to disclose diffuse soft X-ray emission extending up to 2farcm2 (≈0.27 pc) from this binary system. The depth of these XMM-Newton EPIC observations reveals in unprecedented detail the spatial distribution of this diffuse emission, with a bipolar morphology spatially correlated with the optical nebula. The extended X-ray emission shares the same dominant soft X-ray-emitting temperature as the clumps in the jet-like feature resolved by Chandra in the vicinity of the binary system. The harder component in the jet might suggest that the gas cools down; however, the possible presence of nonthermal emission produced by the presence of a magnetic field collimating the mass ejection cannot be discarded. We propose that the ongoing precessing jet creates bipolar cavities filled with X-ray-emitting hot gas that feeds the more extended X-ray bubble as they get disrupted. These EPIC observations demonstrate that the jet feedback mechanism produced by an accreting disk around an evolved, low-mass star can blow hot bubbles, similar to those produced by jets arising from the nuclei of active galaxies. © 2022. The Author(s). Published by the American Astronomical Society., J.A.T. acknowledges support by the Fundación Marcos Moshinsky (Mexico) and UNAM PAPIIT project IA101622 (Mexico). L.S. acknowledges support by UNAM PAPIIT project IN110122 (Mexico). M.A.G. acknowledges the support of grant PGC 2018-102184-B-I00 of the Ministerio de Educación, Innovación y Universidades cofunded with FEDER funds. G.R.-L. acknowledges support from CONACyT grant 263373. Y.H.C. acknowledges the grant MOST 110-2112-M-001-020 from the Ministry of Science and Technology (Taiwan). Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. This work has made extensive use of NASA's Astrophysics Data System., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

We present the first instalment of a deep imaging catalogue containing 58 True, Likely, and Possible extended PNe detected with the Isaac Newton Telescope Photometric H α Survey (IPHAS). The three narrow-band filters in the emission lines of H α, [N ii] λ6584 Å, and [O iii] λ5007 Å used for this purpose allowed us to improve our description of the morphology and dimensions of the nebulae. In some cases even the nature of the source has been reassessed. We were then able to unveil new macro- and micro-structures, which will without a doubt contribute to a more accurate analysis of these PNe. It has been also possible to perform a primary classification of the targets based on their ionization level. A Deep Learning classification tool has also been tested. We expect that all the PNe from the IPHAS catalogue of new extended planetary nebulae will ultimately be part of this deep H α, [N ii], and [O iii] imaging catalogue. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society., LS acknowledges support from PAPIIT grant IN-101819 (Mexico). MAG acknowledges support from grant AYA PGC2018-102184-B-I00 co-funded with FEDER funds. GR-L acknowledges support from CONACyT (grant 263373) and PRODEP (Mexico). JAT acknowledges funding by Dirección General de Asuntos del Personal Academico of the Universidad Nacional Autónoma de México (DGAPA, UNAM) project IA100720 and the Marcos Moshinsky Fundation (Mexico). AAZ acknowledges funding from STFC under grant number ST/T000414/1 and Newton grant ST/R006768/1, and from a Hung Hing Ying visiting professorship at the University of Hong Kong. DNFAI acknowledges funding under ‘Deep Learning for Classification of Astronomical Archives’ from the Newton-Ungku Omar Fund: F08/STFC/1792/2018., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Pulsating and non-pulsating asymptotic giant branch (AGB) stars exhibit a variable near-ultraviolet (near-UV) spectrum, which suggest that mechanisms other than pulsation may affect their near-UV spectrum. In this work, we analyse the near-UV spectra of two groups of AGB stars: (1) regularly pulsating and (2) irregular, small-amplitude stars. Near-UV and blue spectra were obtained for 27 stars distributed into these two groups with the Isaac Newton Telescope (La Palma, Spain). Additional near-UV spectra were taken from the IUE library. The occurrence of Fe II lines depends mainly on the intensity of the stellar continuum: as it increases, Fe II lines are gradually hampered. Balmer emission lines are pulsation driven, as they appear only among the large-amplitude pulsating stars of our sample, between −0.10 < φ < 0.50. Among the regularly pulsating stars, the intensity of the Mg II λ2800 doublet is driven by pulsation, with its maximum between 0.20 < φ < 0.35. On the other hand, this feature is also highly variable among small-amplitude, irregularly pulsating stars. This suggests that, besides pulsation, other mechanisms may participate in the formation of this line. The spectral slope between 3000 < λ(Å), MAG acknowledges support of the grant AYA 2014-57280-P and PGC2018-102184-B-I00, co-funded by European Funds for Regions in Development (FEDER). We acknowledge the ING staff and particularly Lara Monteagudo for the acquisition in service mode of the INT observations presented in this work.

The Mexican energy reform of 2013 enabled the development of new management models and energy infrastructure. However, there is growing and unattended evidence of the weight of human behavior analysis in energy consumption. Therefore, this research integrates, with an interdisciplinary approach, the design of a virtual microgrid and an energy market in the Tonalá Campus of the University of Guadalajara, with real-time energy monitoring and behavior change theories. Firstly, the design of a virtual microgrid of 5 buildings, each with a virtual generation plant, is proposed. Each one dimensioned based on its historical demand and the generation of a 499-kWp photovoltaic plant, installed at the Campus. Both consumption and generation have real-time monitoring installed since May 2018. It was from this data that the virtual power plant for each building was dimensioned. Parallelly, the Transtheoretical Model of the stages of change and the Diffusion of Innovation Theory, are applied to design an intervention to modify energy consumption habits in the Campus community and set the foundations of an energy market pilot program.

Single AGB stars are not normally expected to be X-ray emitters due to the lack of a corona capable of powering a hot plasma. Therefore, the detection of X-ray emission in AGB stars by the ROSAT, Chandra, and XMM-Newton observatories has been interpreted as evidence for binarity. The number of X-ray-emitting AGB stars is, however, very small, and statistically sound conclusions shall be considered tentative. In this paper we aim at increasing the number of X-ray-emitting AGB stars and at providing a consistent analysis of their X-ray emission to be compared to their UV and optical properties. The XMM-Newton 4XMM-DR9 catalog has been searched for X-ray counterparts of various types of AGB stars: nearby (i.e., listed in Hipparcos), mass-losing, and S- and C-types. Seventeen X-ray counterparts of AGB stars have been found in the 4XMM-DR9. Nine of them have pointed XMM-Newton observations, whereas eight are genuine serendipitous discoveries. Together with the AGB stars detected by ROSAT, this increases the number of X-ray AGB stars to 26. Most of their X-ray spectra can be fit by the emission from an optically thin single-temperature thermal plasma with temperatures typically larger than 107 K. There is no obvious correlation between the X-ray and bolometric luminosity of these stars, but the X-ray luminosity generally increases with the amount of far-UV excess. The high temperature of some X-ray-emitting plasma in AGB stars and the correlation of their X-ray luminosity with the far-UV emission supports the origin of this X-ray emission from accretion disks around unseen companions. © 2021. The American Astronomical Society. All rights reserved., M.A.G. acknowledges support of the Spanish Ministerio de Ciencia, Innovacion y Universidades (MCIU) grant PGC2018102184-B-I00. This research made use of the SIMBAD database, operated at the CDS, Strasbourg, France, and the NASA Astrophysics Data System., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Prolactin (PRL) binds its receptor (PRLR) and stimulates cell proliferation, differentiation and survival in prostate cancer (PCa) cell lines via STAT5a, MAPK and AKT.To evaluate the expression of PRL and PRLR in normal and tumor prostate tissues with different Gleason patterns.Samples of normal, benign prostatic hyperplasia and PCa with different Gleason patterns were selected from radical prostatectomy. The intensity, location and percentage of stained cells for PRL and PRLR were evaluated by Immunohistochemistry. Co-localization was observed by confocal microscopy.PRL was expressed diffusely and with a mild intensity in the cytoplasm of normal and tumor prostate luminal cells. Its expression only augmented in the Gleason 3 pattern (p0.0001). The immunostaining intensity and the percentage of positive cells for PRLR did not vary between normal and tumor tissues. However, the location of the PRLR was modified by the tumorigenic process.In non-tumor tissues, PRLR expression was mostly in plasma membrane in the apical zone of epithelial cells. In tumor tissues, it was expressed in intracellular vesicles.The co-localization of PRL and PRLR was demonstrated in normal and tumor tissues suggesting that PRL could be acting in an autocrine and paracrine manner.PRL and its receptor were present in the cytoplasm of the epithelial cells of the normal and tumor prostate gland. In tumor tissues, the change in the location and appearance of cryptic PRLRs that store PRL may keep active the different signaling pathways related to cell proliferation and survival.INTRODUCCIÓN: La prolactina (PRL) se une a su receptor (PRLR) y estimula la proliferación celular, la diferenciación y la supervivencia de la líneas celulares de cáncer de próstata vía STAT5a, MAPK y AKT.OBJETIVO: Evaluar la expresión de la PRL y PRLR en tejido normal y tejido de cáncer de próstata con varios patrones de Gleason.MÉTODOS: Se seleccionaron muestras de tejido benigno, hiperplasia y cáncer de próstata con diferentes patrones de Gleason de prostatectomías radicales. La intensidad, localización y porcentaje de células teñidas por PRL y PRLR fueron evaluadas por immunohistoquimica. La co-localización se observó con microscopio confocal.RESULTADOS: PRL se presentó de forma difusa y con intensidad media en el citoplasma de células luminales normales y de tumor prostático. La expresión solamente aumentó en patrón Gleason 3 (p0,0001). La intensidad de la tinción immunohistoquímica y el porcentaje de células positivas para PRLR no varió entre células normales y tejidos tumorales. Pero, la localización del PRLR fue modificada por el proceso generador del tumor. En tejidos no-tumorales, la expresión de PRLR fue sobre todo en la membrana plasmática en la zona apical de las células epiteliales. En tejidos tumorales, se presentó en las vesículas intracelulares. La co-localizacion de la PRL y PRLR se demostró en tejido normal y tumoral sugeriendo que la PRL funciona con un efecto autocrino y paracrino.CONCLUSIÓN: La PRL y su receptor estuvieron presentes en el citoplasma de células epiteliales de tejido normal y glándula prostática tumoral. En tejidos tumorales, el cambio de localización y la apariencia cripticas del PRLR que guarda la PRL debe mantener activos los diferentes caminos de señalización relacionados con la proliferación celular y la supervivencia.

We present a multiwavelength characterization of the planetary nebula (PN) NGC 6905 and its [Wolf–Rayet]-type ([WR]) central star (CSPN) HD 193949. Our Nordic Optical Telescope Alhambra Faint Object Spectrograph and Camera (ALFOSC) spectra and images unveil in unprecedented detail the high-ionization structure of NGC 6905. The high-quality spectra of HD 193949 allowed us to detect more than 20 WR features including the characteristic O-bump, blue bump, and red bump, which suggests a spectral type no later than a [WO2]-subtype. Moreover we detect the Ne VII and Ne VIII broad emission lines, rendering HD 193949 yet another CSPN with Teff ≲ 150 kK exhibiting such stellar emission lines. We studied the physical properties (Te and ne) and chemical abundances of different regions within NGC 6905 including its low-ionization clumps; abundances are found to be homogeneous. We used the PoWR stellar atmosphere code to model the spectrum of HD 193949, which is afterwards used in a photoionization model performed with CLOUDY that reproduces the nebular and dust properties for a total mass in the 0.31–0.47 M⊙ range and a mass of C-rich dust of ∼2 × 10−3 M⊙. Adopting a current stellar mass of 0.6 M⊙, our model suggests an initial mass ∼1 M⊙ for HD 193949, consistent with the observations. © 2021 The Author(s)., VMAGG acknowledges support from the Programa de Becas posdoctorales of the Dirección General de Asuntos del Personal Académico of the Universidad Nacional Autónoma de México (DGAPA, UNAM, Mexico). VMAGG and JAT acknowledge funding by DGAPA UNAM PAPIIT project IA100720. JAT also acknowledges support from the Marcos Moshinsky Fundation (Mexico). GR acknowledge support from Consejo Nacional de Ciencia y Tecnología (CONACYT) for student scholarship. MAG acknowledges support of the Spanish Ministerio de Ciencia, Innovación y Universidades grant PGC2018-102184-B-I00, cofunded by FEDER funds. LS acknowledges funding by DGAPA UNAM PAPIIT project IN-101819. GR-L acknowledges support from CONACYT grant 263373 and PRODEP (Mexico). This work is based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos in La Palma, Spain, of the Instituto de Astrofisica de Canarias. This work uses public data from the IR telescope Spitzer Space Telescope through the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory at the California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). WISE is a joint project of the University of California (Los Angeles, USA) and the JPL/Caltech. The Infrared Astronomical Satellite (IRAS) was a joint project of the US, UK, and the Netherlands. This research is based on observations with AKARI, a JAXA project with the participation of ESA. This work has make extensive use of the NASA’s Astrophysics Data System., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The guest star of AD 1181 is the only historical supernova of the past millennium that is without a definite counterpart. The previously proposed association with supernova remnant G130.7+3.1 (3C 58) is in strong doubt because of the inferred age of this remnant. Here we report a new identification of SN 1181 with our codiscovery of the hottest known Wolf-Rayet star of the oxygen sequence (IRAS 00500+6713 or 2MASS J00531123+6730023, here named by us as "Parker's star") and its surrounding nebula Pa 30. Our spectroscopy of the nebula shows a fast shock with extreme velocities of ≈1100 km s-1. The derived expansion age of the nebula implies an explosive event ≈1000 yr ago that agrees with the 1181 event. The on-sky location also fits the historical Chinese and Japanese reports of SN 1181 to within 3.°5. Pa 30 and Parker's star have previously been proposed to be the result of a double-degenerate merger, leading to a rare Type Iax supernova. The likely historical magnitude and the distance suggest the event was subluminous for normal supernova. This agrees with the proposed Type Iax association that would also be only the second of its kind in the Galaxy. Taken together, the age, location, event magnitude, and duration elevate Pa 30 to prime position as the counterpart of SN 1181. This source is the only Type Iax supernova where detailed studies of the remnant star and nebula are possible. It provides strong observational support for the double-degenerate merger scenario for Type Iax supernovae. © 2021. The Author(s). Published by the American Astronomical Society., Q.A.P. thanks the Hong Kong Research Grants Council for GRF research support under grants 17326116 and 17300417. A.R. and F.L. thank HKU for the provision of postdoctoral fellowships under Q.A.P., while F.L. also acknowledges funding from MTA Hungary (OTKA project No. K-132406). A.A.Z. thanks the Hung Hing Ying Foundation for the provision of a visiting professorship at HKU and acknowledges funding from the UK STFC under grant ST/T000414/1. M.A.G. was funded under grant number PGC2018-102184-B-I00 of the Ministerio de Educación, Innovación y Universidades cofunded with FEDER funds., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

With an effective temperature of ≃200,000 K, KPD 0005+5106 is one of the hottest white dwarfs (WDs). ROSAT unexpectedly detected "hard"(∼1 keV) X-rays from this apparently single WD. We have obtained Chandra observations that confirm the spatial coincidence of this hard X-ray source with KPD 0005+5106. We have also obtained XMM-Newton observations of KPD 0005+5106, as well as PG 1159-035 and WD 0121-756, which are also apparently single and whose hard X-rays were detected by ROSAT at 3σ-4σ levels. The XMM-Newton spectra of the three WDs show remarkably similar shapes that can be fitted by models including a blackbody component for the stellar photospheric emission, a thermal plasma emission component, and a power-law component. Their X-ray luminosities in the 0.6-3.0 keV band range from 4 × 1029 to 4 × 1030 erg s-1. The XMM-Newton EPIC-pn soft-band (0.3-0.5 keV) light curve of KPD 0005+5106 is essentially constant, but the hard-band (0.6-3.0 keV) light curve shows periodic variations. An analysis of the generalized Lomb-Scargle periodograms for the XMM-Newton and Chandra hard-band light curves finds a convincing modulation (false-alarm probability of 0.41%) with a period of 4.7 ± 0.3 hr. Assuming that this period corresponds to a binary orbital period, the Roche radii of three viable types of companion have been calculated: M9V star, T brown dwarf, and Jupiter-like planet. Only the planet has a size larger than its Roche radius, although the M9V star and T brown dwarf may be heated by the WD and inflate past the Roche radius. Thus, all three types of companion may be donors to fuel accretion-powered hard X-ray emission. © 2021. The American Astronomical Society. All rights reserved., This research was supported by the NASA grants SAO GO8-9026 (Chandra) and JPL 1319342 (Spitzer). Y.H.C. acknowledges grants MOST 108-2112-M001-045 and MOST 109-2112-M-001-040 from the Ministry of Science and Technology of Taiwan, Republic of China. J.A.T. and M.A.G. are funded by UNAM DGAPA PAPIIT project IA100318. M.A.G. also acknowledges support from grant PGC2018-102184-B-IOO of the Spanish Ministerio de Ciencia, Educacion y Universidades cofunded by FEDER funds. This paper has used observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

We present the analysis of XMM–Newton European Photon Imaging Camera (EPIC) observations of the nova shell IPHASX J210204.7+471015. We detect X-ray emission from the progenitor binary star with properties that resemble those of underluminous intermediate polars such as DQ Herculis (DQ Her): an X-ray-emitting plasma with temperature of TX = (6.4 ± 3.1) × 106 K, a non-thermal X-ray component, and an estimated X-ray luminosity of LX = 1030 erg s−1. Time series analyses unveil the presence of two periods, the dominant with a period of 2.9 ± 0.2 h, which might be attributed to the spin of the white dwarf, and a secondary of 4.5 ± 0.6 h that is in line with the orbital period of the binary system derived from optical observations. We do not detect extended X-ray emission as in other nova shells probably due to its relatively old age (130–170 yr) or to its asymmetric disrupted morphology that is suggestive of explosion scenarios different to the symmetric ones assumed in available numerical simulations of nova explosions. © 2021 The Author(s)., The authors thank the referee for a prompt report. JAT acknowledges support from the Fundación Marcos Moshinsky (Mexico). JAT is funded by PAPIIT project IA100720 of the Direccion General de Asuntos del Personal Academico of the Universidad Nacional Autonoma de México (DGAPA, UNAM). ES and GR are thankful to Consejo Nacional de Ciencia y Tecnología (CONACyT -México) for their student grants. MAG acknowledges support of the Spanish Ministerio de Ciencia, Innovación y Universidades (MCIU) grant PGC2018-102184-B-I00 and the State Agency for Research of the Spanish MCIU through the `Center of Excellence Severo Ochoa' award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). GR-L acknowledges support from CONACYT grant 263373. LS acknowledges support from PAPIIT-UNAM grant IN101819. This work has made extensive use of NASA's Astrophysics Data System (ADS).

A correction has been published: Monthly Notices of the Royal Astronomical Society, Volume 509, Issue 2, January 2022, Page 2896, https://doi.org/10.1093/mnras/stab3247, We present a comprehensive analysis of the compact planetary nebula M 2-31 investigating its spectral properties, spatio-kinematical structure, and chemical composition using Gran Telescopio Canarias (GTC) Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía (MEGARA) integral field spectroscopic observations and Nordic Optical Telescope(NOT) Alhambra Faint Object Spectrograph and Camera (ALFOSC) medium-resolution spectra and narrow-band images. The GTC MEGARA high-dispersion observations have remarkable tomographic capabilities, producing an unprecedented view of the morphology and kinematics of M 2-31 that discloses a fast spectroscopic bipolar outflow along position angles 50° and 230°, an extended shell, and a toroidal structure or waist surrounding the central star perpendicularly aligned with the fast outflows. These observations also show that the C ii emission is confined in the central region and enclosed by the [N ii] emission. This is the first time that the spatial segregation revealed by a two-dimensional map of the C ii line implies the presence of multiple plasma components. The deep NOT ALFOSC observations allowed us to detect broad Wolf-Rayet (WR) features from the central star of M 2-31, including previously undetected broad O vi lines that suggest a reclassification as a [WO4]-type star. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society., JSRG and VMAGG acknowledge support from the Programas de Beca Posdoctorales funded by Dirección General de Asuntos del Personal Académico of the Universidad Nacional Autónoma de México (DGAPA, UNAM). JAT acknowledges funding by DGAPA, UNAM PAPIIT project IA100720 and the Marcos Moshinsky Foundation (Mexico). SC and MAG acknowledge financial support from State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). MAG acknowledges support of the Spanish Ministerio de Ciencia, Innovación y Universidades (MCIU) grant PGC2018-102184-B-100. LS acknowledges support from PAPIIT-UNAM grant IN101819. GR-L acknowledges support from CONACYT (grant 263373) and PRODEP (Mexico). The GTC Science Operations group is recognized for scheduling the GTC MEGARA observations beneath the exacting conditions requested by this program.

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The INT Photometric Hα Survey (IPHAS) has provided us with a number of new emission-line sources, among which planetary nebulae (PNe) constitute an important fraction. Here we present a detailed analysis of the IPHAS nebula Sab 19 (IPHASX J055242.8+262116) based on radio, infrared, and optical images and intermediate- and high-dispersion long-slit spectra. Sab 19 consists of a roundish 0.10 pc in radius double-shell nebula surrounded by a much larger 2.8 pc in radius external shell with a prominent H-shaped filament. We confirm the nature of the main nebula as a PN whose sub-solar N/O ratio abundances, low ionized mass, peculiar radial velocity, and low-mass central star allow us to catalogue it as a Type III PN. Apparently, the progenitor star of Sab 19 became a PN when crossing the Perseus Arm during a brief visit of a few Myr. The higher N/O ratio and velocity shift ≃ 40 km s-1 of the external shell with respect to the main nebula and its large ionized mass suggest that it is not truly associated with Sab 19, but it is rather dominated by a Strömgren zone in the interstellar medium ionized by the PN central star. © The Author(s) 2020. Published by Oxford University Press on behalf of The Royal Astronomical Society., We acknowledge support of the publication fee by the CSIC Open Access Publication Support Initiative through its Unit of Information Resources for Research (URICI). MAG acknowledges support from the Spanish Government Ministerio de Ciencia, Innovacion y Universidades (MCIU) through grant PGC2018-102184-B-I00, LS acknowledges support from DGAPA, UNAM PAPIIT project IN101819, GR-L acknowledges support from Consejo Nacional de Ciencia y Tecnologia (CONACyT) grant 263373 and Programa para el Desarrollo Profesional (PRODEP) Mexico, and EJA acknowledges support from MCIU grant PGC2018-095049-B-C21. MAG and EJA are supported by the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This research has made use of the SIMBAD database operated at CDS (Strasbourg, France), the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology, the NASA's Astrophysics Data System, and NRAO VLA Sky Survey. It has also made use of data obtained as part of the INT Photometric Ha Survey (IPHAS) of the Northern Galactic Plane carried out at the Isaac Newton Telescope (INT), which is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof ' isica de Canarias. All IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge. Based on observations made with the Nordic Optical Telescope (NOT) and Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. NOT is owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University. This work is partly based on data obtained with the instruments ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA, and OSIRIS, built by a Consortium led by the Instituto de Astrofisica de Canarias in collaboration with the Instituto de Astronomia of the Universidad Autonoma de México. OSIRIS was funded by GRANTECAN and the National Plan of Astronomy and Astrophysics of the Spanish Government.

Jets (fast collimated outflows) are claimed to be the main shaping agent of the most asymmetric planetary nebulae (PNs), as they impinge on the circumstellar material at late stages of the asymptotic giant branch phase. The first jet detected in a PN was that of NGC 2392, yet there is no available image because of its low surface brightness contrast with the bright nebular emission. Here we take advantage of the tomographic capabilities of Gran Telescopio de Canarias Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía high-dispersion integral field spectroscopic observations of the jet in NGC 2392 to gain unprecedented details of its morphology and kinematics. The jet of NGC 2392 is found to emanate from the central star, break through the walls of the inner shell of this iconic PN and extend outside the nebula's outermost regions with an S-shaped morphology suggestive of precession. At odds with the fossil jets found in mature PNs, the jet in NGC 2392 is currently being collimated and launched. The high nebular excitation of NGC 2392, which implies an He++/He ionization fraction too high to be attributed to the known effective temperature of the star, has been proposed in the past to hint at the presence of a hot white dwarf companion. In conjunction with the hard X-ray emission from the central star, the present-day jet collimation would support the presence of such a double-degenerate system where one component undergoes accretion from a remnant circumbinary disk of the common envelope phase. © 2021. The American Astronomical Society. All rights reserved., Ministerio de Ciencia, Innovacion y Universidades (MCIU) grant PGC2018-102184-B-I00. M.A.G., S.C., and B.M.M. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). G.R.-L. acknowledges support from CONACyT (grant 263373) and PRODEP (Mexico). J.S.R.G. and V.M.A.G.G. acknowledge support from the Programa de Becas posdoctorales funded by Direccion General de Asuntos del Personal Academico (DGAPA) of the Universidad Nacional Autonoma de Mexico (UNAM). J.A.T. acknowledges funding by DGAPA UNAM PAPIIT project IA100720 and the Marcos Moshinsky Foundation (Mexico). X. F. acknowledges support by the Strategic Priority Research Program of Chinese Academy of Sciences, grant No. XDB 41000000.

We present the first detailed study of the bipolar planetary nebula (PN) IPHASX J191104.8+060845 (PN G 040.6-01.5) discovered as part of the Isaac Newton Telescope Photometric Hα Survey of the Northern Galactic plane (IPHAS). We present Nordic Optical Telescope narrow-band images to unveil its true morphology. This PN consists of a main cavity with two newly uncovered extended low-surface brightness lobes located towards the NW and SE directions. Using near-IR WISE images we unveiled the presence of a barrel-like structure, which surrounds the main cavity, which would explain the dark lane towards the equatorial regions. We also use Gran Telescopio de Canarias spectra to study the physical properties of this PN. We emphasize the potential of old PNe detected in IPHAS to study the final stages of the evolution of the circumstellar medium around solar-like stars. © 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society, The authors are thankful to the referee for a prompt report that improved the presentation of this paper. JBJ-G and JAT are funded by UNAM DGAPA PAPIIT projects IA100318 and IA100720. JBJ-G and LS are funded by UNAM-PAPIIT grant IN101819. SZ works under the collaboration agreement 'UNAM-TecNM 433103020-30-IX-15'. GR-L acknowledges support from CONACYT grant 263373 and PRODEP (Mexico). MAG acknowledges support from the Spanish Government Ministerio de Ciencia, Innovacion y Universidades through grant PGC2018-102184-B-I00. QAP thanks the Hong Kong Research Grants Council for GRF research support under grants 17326116 and 17300417. We thank the daytime and night support staff at the OAN-SPM for facilitating and helping obtain our observations. This paper makes use of data obtained as part of the INT Photometric Ha Survey of the Northern Galactic Plane (IPHAS) carried out at the Isaac Newton Telescope (INT). The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge. Based on observations collected at the Observatorio Astronomico Nacional at San Pedro Martir, B.C., Mexico. Based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

We present a detailed analysis of the new planetary nebula (PN) IPHASX J193718.6+202102 using deep imaging and intermediate- and high-resolution spectroscopy that are interpreted through morpho-kinematic and photoionization modelling. The physical structure of the nebula consists of a fragmented torus and an extremely faint orthogonal bipolar outflow, contrary to the pinched waist PN morphology suggested by its optical image. Our kinematic analysis indicates that the torus is expanding at 25 ± 5 km s-1 and is gradually breaking up. At an estimated distance of 7.1-0.3+0.8 kpc, the corresponding kinematic age of ∼26 000 yr is consistent with a faint and disintegrating PN. The intermediate-resolution spectra reveal an excited PN with chemical abundances typical of Type II PNe. Based on the latter, we also estimate an initial mass for the progenitor in the range 2-3 M⊙ and a central star (CSPN) mass MCSPN ∼0.61 M⊙. The Spitzer MIPS 24 μm emission that closely follows the fragmented torus could be attributed to the emission of [O iv] at 25.9 μm rather than to dust emission. All the results coherently point towards an evolved moderately massive bipolar Type II PN on the brink of dissolving into the interstellar medium. © 2020 The Author(s)., The authors are thankful to the referees for their comments that improved this paper. LS acknowledges support from UNAM DGAPA PAPIIT project IN101819 (Mexico). MAG acknowledges support from grant AYA PGC2018-102184-B-I00 co-funded with FEDER funds. SZ works under the collaboration agreement ‘UNAM-TecNM 43310-3020-30-IX-15’. JAT and MAG are funded by UNAM DGAPA PAPIIT project IA100720. GRL acknowledges support from CONACYT (grant 263373) and PRODEP (Mexico). This work is partially based on observations collected at the Observatorio Astronómico Nacional at San Pedro Mártir, B.C., Mexico and we thank the daytime and night support staff at the OAN-SPM for facilitating and helping obtain our observations. Based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association, and the Gran Telescopio Canarias (GTC), both installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias in La Palma, Spain. This paper makes use of data obtained as part of the INT Photometric H α Survey of the Northern Galactic Plane (IPHAS, www.iphas.org) carried out at the Isaac Newton Telescope (INT). The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge. The bandmerged DR2 catalogue was assembled at the Centre for Astrophysics Research, University of Hertfordshire, supported by STFC grant ST/J001333/1. The OSN director is acknowledged for awarding observations through a DDT programme and the telescope operator Alfredo Sota for conducting the observations. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. In memoriam of Johannes Andersen, director of the NOT from 2002 to 2013.

The Stingray Nebula, a.k.a. Hen3-1357, appeared for the first time in 1990 when bright nebular lines and radio emission that had not been observed before were unexpectedly discovered. In the ensuing years, the nebula faded precipitously. We report changes in shape and large decreases in its nebular emission-line fluxes based on well-calibrated images obtained by the Hubble Space Telescope in 1996 and 2016. Hen3-1357 is now a "recombination nebula." © 2021. The American Astronomical Society. All rights reserved., M.A.G. acknowledges financial support by grant PGC2018-102184-B-I00, cofunded with FEDER funds. G.R.-L. acknowledges financial support from CONACyT grant 263373. We thank D. Schonberner for very useful insights. B.B. thanks Gunther Cibis for informing him that although they are surrounded by ionized gas, K 2-2, GD 561, PHL 932, and DeHt5 are probably not true PNe., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Full list of authors: Bonoli, S.; Marín-Franch, A.; Varela, J.; Vázquez Ramió, H.; Abramo, L. R.; Cenarro, A. J.; Dupke, R. A.; Vílchez, J. M.; Cristóbal-Hornillos, D.; González Delgado, R. M.; Hernández-Monteagudo, C.; López-Sanjuan, C.; Muniesa, D. J.; Civera, T.; Ederoclite, A.; Hernán-Caballero, A.; Marra, V.; Baqui, P. O.; Cortesi, A.; Cypriano, E. S.; Daflon, S.; de Amorim, A. L.; Díaz-García, L. A.; Diego, J. M.; Martínez-Solaeche, G.; Pérez, E.; Placco, V. M.; Prada, F.; Queiroz, C.; Alcaniz, J.; Alvarez-Candal, A.; Cepa, J.; Maroto, A. L.; Roig, F.; Siffert, B. B.; Taylor, K.; Benitez, N.; Moles, M.; Sodré, L.; Carneiro, S.; Mendes de Oliveira, C.; Abdalla, E.; Angulo, R. E.; Aparicio Resco, M.; Balaguera-Antolínez, A.; Ballesteros, F. J.; Brito-Silva, D.; Broadhurst, T.; Carrasco, E. R.; Castro, T.; Cid Fernandes, R.; Coelho, P.; de Melo, R. B.; Doubrawa, L.; Fernandez-Soto, A.; Ferrari, F.; Finoguenov, A.; García-Benito, R.; Iglesias-Páramo, J.; Jiménez-Teja, Y.; Kitaura, F. S.; Laur, J.; Lopes, P. A. A.; Lucatelli, G.; Martínez, V. J.; Maturi, M.; Overzier, R. A.; Pigozzo, C.; Quartin, M.; Rodríguez-Martín, J. E.; Salzano, V.; Tamm, A.; Tempel, E.; Umetsu, K.; Valdivielso, L. ; von Marttens, R.; Zitrin, A.; Díaz-Martín, M. C.; López-Alegre, G.; López-Sainz, A.; Yanes-Díaz, A.; Rueda-Teruel, F.; Rueda-Teruel, S.; Abril Ibañez, J.; L Antón Bravo, J.; Bello Ferrer, R.; Bielsa, S.; Casino, J. M.; Castillo, J.; Chueca, S.; Cuesta, L.; Garzarán Calderaro, J.; Iglesias-Marzoa, R.; Íniguez, C.; Lamadrid Gutierrez, J. L.; Lopez-Martinez, F.; Lozano-Pérez, D.; Maícas Sacristán, N.; Molina-Ibáñez, E. L.; Moreno-Signes, A.; Rodríguez Llano, S.; Royo Navarro, M.; Tilve Rua, V.; Andrade, U.; Alfaro, E. J.; Akras, S.; Arnalte-Mur, P.; Ascaso, B.; Barbosa, C. E.; Beltrán Jiménez, J.; Benetti, M.; Bengaly, C. A. P.; Bernui, A.; Blanco-Pillado, J. J.; Borges Fernandes, M.; Bregman, J. N.; Bruzual, G.; Calderone, G.; Carvano, J. M.; Casarini, L.; Chaves-Montero, J.; Chies-Santos, A. L.; Coutinho de Carvalho, G.; Dimauro, P.; Duarte Puertas, S.; Figueruelo, D.; González-Serrano, J. I.; Guerrero, M. A.; Gurung-López, S.; Herranz, D.; Huertas-Company, M.; Irwin, J. A.; Izquierdo-Villalba, D.; Kanaan, A.; Kehrig, C.; Kirkpatrick, C. C.; Lim, J.; Lopes, A. R.; Lopes de Oliveira, R.; Marcos-Caballero, A.; Martínez-Delgado, D.; Martínez-González, E.; Martínez-Somonte, G.; Oliveira, N.; Orsi, A. A.; Penna-Lima, M.; Reis, R. R. R.; Spinoso, D.; Tsujikawa, S.; Vielva, P.; Vitorelli, A. Z.; Xia, J. Q.; Yuan, H. B.; Arroyo-Polonio, A.; Dantas, M. L. L.; Galarza, C. A.; Gonçalves, D. R.; Gonçalves, R. S.; Gonzalez, J. E.; Gonzalez, A. H.; Greisel, N.; Jiménez-Esteban, F.; Landim, R. G.; Lazzaro, D.; Magris, G.; Monteiro-Oliveira, R.; Pereira, C. B.; Rebouças, M. J.; Rodriguez-Espinosa, J. M.; Santos da Costa, S.; Telles, E., The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will scan thousands of square degrees of the northern sky with a unique set of 56 filters using the dedicated 2:55m Javalambre Survey Telescope (JST) at the Javalambre Astrophysical Observatory. Prior to the installation of the main camera (4:2 deg2 field-of-view with 1.2 Gpixels), the JST was equipped with the JPAS-Pathfinder, a one CCD camera with a 0:3 deg2 field-of-view and plate scale of 0.23 arcsec pixel?1. To demonstrate the scientific potential of J-PAS, the JPAS-Pathfinder camera was used to perform miniJPAS, a _1 deg2 survey of the AEGIS field (along the Extended Groth Strip). The field was observed with the 56 J-PAS filters, which include 54 narrow band (FWHM _ 145 ) and two broader filters extending to the UV and the near-infrared, complemented by the u; g; r; i SDSS broad band filters. In this miniJPAS survey overview paper, we present the miniJPAS data set (images and catalogs), as we highlight key aspects and applications of these unique spectro-photometric data and describe how to access the public data products. The data parameters reach depths of magAB ' 22?23:5 in the 54 narrow band filters and up to 24 in the broader filters (5_ in a 300 aperture). The miniJPAS primary catalog contains more than 64 000 sources detected in the r band and with matched photometry in all other bands. This catalog is 99% complete at r = 23:6 (r = 22:7) mag for point-like (extended) sources. We show that our photometric redshifts have an accuracy better than 1% for all sources up to r = 22:5, and a precision of _0:3% for a subset consisting of about half of the sample. On this basis, we outline several scientific applications of our data, including the study of spatially-resolved stellar populations of nearby galaxies, the analysis of the large scale structure up to z _ 0:9, and the detection of large numbers of clusters and groups. Sub-percent redshift precision can also be reached for quasars, allowing for the study of the large-scale structure to be pushed to z 2. The miniJPAS survey demonstrates the capability of the J-PAS filter system to accurately characterize a broad variety of sources and paves the way for the upcoming arrival of J-PAS, which will multiply this data by three orders of magnitude. © 2021 EDP Sciences. All rights reserved., Funding for OAJ, UPAD, and CEFCA has been provided by the Governments of Spain and Aragon through the Fondo de Inversiones de Teruel; the Aragon Government through the Research Groups E96, E103, and E16_17R; the Spanish Ministry of Science, Innovation and Universities (MCIU/AEI/FEDER, UE) with grant PGC2018-097585-B-C21; the Spanish Ministry of Economy and Competitiveness (MINECO/FEDER, UE) under AYA2015-66211-C2-1-P, AYA2015-66211-C2-2, AYA2012-30789, and ICTS2009-14; and European FEDER funding (FCDD10-4E-867, FCDD13-4E-2685). This work has made used of CEFCA's Scientific High Performance Computing system which has been funded by the Governments of Spain and Aragon through the Fondo de Inversiones de Teruel, and the Spanish Ministry of Economy and Competitiveness (MINECO-FEDER, grant AYA2012-30789). Funding for the J-PAS project has been provided also by the Brazilian agencies FINEP, FAPESP, FAPERJ and by the National Observatory of Brazil. Additional funding was also provided by the Tartu Observatory and by the Chinese Consortium from the Academy of Sciences SB acknowledges partial support from the project PGC2018-097585-B-C22. R.A.D. acknowledges support from the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico -CNPq through BP grant 308105/2018-4, and the Financiadora de Estudos e Projetos -FINEP grants REF. 1217/13 -01.13.0279.00 and REF 0859/10 -01.10.0663.00 and also FAPERJ PRONEX grant E-26/110.566/2010 for hardware funding support for the J-PAS project through the National Observatory of Brazil and Centro Brasileiro de Pesquisas Fisicas. LRA acknowledges financial support from CNPq (306696/2018-5) and FAPESP (2015/17199-0). VMthanks CNPq (Brazil) and FAPES (Brazil) for partial financial support and the H2020 project No 888258. L.A.D.G. and K.U. acknowledge support from the Ministry of Science and Technology of Taiwan (grant MOST 106-2628-M-001-003-MY3) and from the Academia Sinica (grant AS-IA-107-M01). J.M.D. and D.H acknowledge the support of project PGC2018-101814-B-100. MQ thanks CNPq (Brazil) and FAPERJ (Brazil) for financial support. PC acknowledges financial support from FAPESP (2018/05392-8) and CNPq (310041/2018-0). AAC acknowledges support from FAPERJ (E26/203.186/2016), CNPq (304971/2016-2 and 401669/2016-5), and the Universidad de Alicante (contract UATALENTO1802). C.Q. acknowledges support from FAPESP (2015/11442-0 and 2019/067661). V.M.P. is supported by NOIRLab, which is managed by AURA under a cooperative agreement with the NSF. P.B acknowledges support from CAPES -Finance Code 001. IAA researchers acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). Authors acknowledge support from the Generalitat Valenciana project of excellence Prometeo/2020/085. RGD, GMS, JRM, RGB, EP acknowledge financial support from the project AyA2016-77846-P. TC is supported by the INFN INDARK PD51 and PRIN-MIUR 2015W7KAWC. MAR and ALM acknowledge support from the MINECO project FIS2016-78859P(AEI/FEDER, UE). ET, AT and JL acknowledge the support by ETAg grants IUT40-2 and by EU through the ERDF CoE grant TK133 and MOBTP86. CK, JMV, JIP acknowledge financial support from project AYA2016-79724C4-4P. PAAL thanks the support of CNPq (309398/2018-5). LC thanks CNPq for partial support. Y.J-T acknowledges financial support from the FAPERJ (E26/202.835/2016), and from the Horizon 2020 Marie Sklodowska-Curie grant agreement No 898633. DMD acknowledges financial support from the SFB 881 of the DFG and from the MINECO grant AYA2016-81065-C2-2. FP acknowledges support of the project PGC2018-101931-B-I00. JC acknowledges support of the project E AYA2017-88007-C3-1-P, and co-financed by the FEDER. JIGs acknowledges support of projects of reference AYA2017-88007-C3-3-P, and PGC2018-099705-B-I00 and co-financed by the FEDER. EMG and PV would like to acknowledge financial support from the project ESP2017-83921C2-1-R. GMS acknowleges financial support from a predoctoral contract, ref. PRE2018-085523 (MCIU/AEI/FSE, UE). S.C. is partially supported by CNPq. R.G.L. acknowledges CAPES (process 88881.162206/2017-01) and Alexander von Humboldt Foundation for the financial support. JSA acknowledges support from FAPERJ (E26/203.024/2017), CNP (310790/2014-0 and 400471/2014-0) and FINEP (1217/13 -01.13.0279.00 and Ref. 0859/10 -01.10.0663.00). RvM acknowledges support from CNPq. AFS, PAM, VJM and FJB acknowledge support from project AYA2016-81065-C2-2. PAM acknowledges support from the "Subprograma Atraccio de Talent -Contractes Postdoctorals de la Universitat de Valencia". ESC acknowledges support from CNPq (308539/20184) and FAPESP (2019/19687-2). CMdO acknowledges support from CNPq (grant 312333/2014-5) and FAPESP (grant 2009/54202-8). LSJ acknowledges support from CNPq (grant 304819/2017-4) and FAPESP (grant 2012/008004). JMC acknowledges support from CNPq (grant 310727/2016-2). C.H.-M. and N. Greisel also acknowledge the support of the European Union via the Career Integration Grant CIG-PCIG9-GA-2011-294183. JJBP and AMC would like to acknowledge the support from the grant PGC2018-094626-B-C21 and the Basque Government grant IT-979-16. AMC acknowledges the postdoctoral contract from the University of the Basque Country UPV/EHU "Especializacioon de personal investigador doctor" program. MLLD acknowledges CAPES -Finance Code 001; and CNPq (142294/2018-7). GB acknowledges financial support from the UNAM through grant DGAPA/PAPIIT IG100319, from CONACyT through grant CB2015-252364, and from FAPESP projects 2017/02375-2 and 2018/05392-8. M.J. Reboucas acknowledges the support of FAPERJ under a CNE E-26/202.864/2017 grant, and CNPq. Support by CNPq (305409/2016-6) and FAPERJ (E-26/202.841/2017) is acknowledged by DL. AB acknowledges a CNPq fellowship. C.A.G.acknowledges support from CAPES. EA acknowledges support from FAPESP (2011/18729-1). AC acknowledges support from PNPD/CAPES. ABA and FSK acknowledge the Severo Ochoa program SEV-2015-0548. FSK also thanks the AYA2017-89891-P and the RYC2015-18693 grants. DF acknowledges support from the Atraccion del Talento Cientifico en Salamanca programme and the project PGC2018-096038B-I00.

We present the analysis of the planetary nebula (PN) NGC 2371 around the [Wolf-Rayet] (WR) star WD 0722+295. Our Isaac Newton Telescope intermediate dispersion spectrograph spectra, in conjunction with archival optical and ultraviolet images, unveil in unprecedented detail the high ionization of NGC 2371. The nebula has an apparent multipolar morphology, with two pairs of lobes protruding from a barrel-like central cavity, a pair of dense low ionization knots misaligned with the symmetry axis embedded within the central cavity, and a high-excitation halo mainly detected in He ii. The abundances from the barrel-like central cavity and dense knots agree with abundance determinations for other PNe with [WR]-type central stars of PNe. We suggest that the densest knots inside NGC 2371 are the oldest structures, remnant of a dense equatorial structure, while the main nebular shell and outer lobes resulted from a latter ejection that ended the stellar evolution. The analysis of position-velocity diagrams produced from our high-quality spectra suggests that NGC 2371 has a bipolar shape with each lobe presenting a double structure protruding from a barrel-like central region. The analysis of the spectra of WD 0722+295 results in similar stellar parameters as previously reported. We corroborate that the spectral subtype corresponds with a [WO1] type. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society., VMAGG, JAT, MAG, and HT are funded by Dirección General de Asuntos del Personal Académico (DGAPA), Universidad Nacional Autónoma de México (UNAM) PAPIIT project IA100318. GRL acknowledges support from Fundación Marcos Moshinsky, Consejo Nacional de Ciencia y Tecnología (CONACYT), and Programa para el Desarrollo Profe-sional Docente (PRODEP) (Mexico). MAG acknowledges support of the Spanish Ministerio de Ciencia, Innovación y Universidades grant PGC2018-102184-B-I00, cofunded by FEDER funds. LS thanks support from UNAM PAPIIT grant IN101819. YDM thanks CONACYT for the research grant CB-A1-S-25070. This work has make extensive use of the NASA’s Astrophysics Data System. This paper also presents data obtained with the MOS camera at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. The authors thank E. Santamaría for helping produce the velocity sketch of NGC 2371. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

We present a multiwavelength study of the iconic Bubble Nebula (NGC 7635) and its ionizing star BD+60 degrees 2521 We obtained XMM Newton EPIC X-ray observations to search for. extended X-ray emission as in other similar wind-blown bubbles around massive stars. We also obtained San Pedro Madir spectroscopic observations with. the Manchester Echelle Spectrometer to study the dynamics of the Bubble Nebula. Although our EPIC observations are deep, we do not detect extended X-ray emission from this wind-blown bubble. On the other hand, BD+60 degrees 2522 is a bright X-ray source similar to other 0 stars. We used the stellar atmosphere code PolATR to characterize BD+60 degrees 2522 and found that this star is a young O-type star with stellar wind capable of producing a wirid-blown bubble that in principle could be filled with hot gas. We discussed our findings in line with recent ntirnerical simulations'proposing that the Bubble Nebula has been formed as the result of the fast motion of BD+60 degrees 2522 through the medium. Our kinematic study shows that the Bubble Nebula is composed by a series of nested shells, some showing blister-like structures, but with little signatures of hydrodynamical instabilities that would mix the material producing diffuse X-ray emission as seen in other wind-blown bubbles. Its morphology seems to be merely the result of projection effects of these different shells. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society, This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The NOT data presented were obtained with ALFOSC and FIES, which are provided by the Instituto de Astroffsica de Andalucfa (IAA-CSIC) under ajoint agreement with the University of Copenhagen and NOTSA. This paper makes use of observations carried out at the Observatorio Astronomico Nacional on the Sierra San Pedro Mdfrtir (OAN-SPM), Baja California, Mexico. We thank the daytime and night support staff at the OAN-SPM for facilitating and helping obtain our observations. JAT, MAG, and HT are funded by UNAM DGAPA PAPIIT projects IA100318 and IA100720. GRL acknowledges support from Fundacion Marcos Moshinsky, CONACyT, and PRODEP (Mexico). MAG acknowledges support of the grants AYA 201457280-P and PGC2018-102184-B-I00 of the Spanish Ministerio de Ciencia, Innovacion y Universidades, cofunded with FEDER funds. LS is supported by Direccion General de Asuntos del Personal Acadmico, Universidad Nacional Autonoma de Mexico project IN101819.

Nova shells can provide important information on their distance, their interactions with circumstellar and interstellar media, and the evolution in morphology of the ejecta. We have obtained narrowband images of a sample of five nova shells, namely DQ Her, FH Ser, T Aur, V476 Cyg, and V533 Her, with ages ranging from 50 to 130 yr. These images have been compared with suitable available archival images to derive their angular expansion rates. We find that all the nova shells in our sample are still in the free expansion phase, which can be expected, as the mass of the ejecta is 7-45 times larger than the mass of the swept-up circumstellar medium. The nova shells will keep expanding freely for time periods up to a few hundred years, reducing their time dispersal into the interstellar medium. © 2020. The American Astronomical Society. All rights reserved., E.S., G.R., and J.A.Q.M. acknowledge support from CONACyT and Universidad de Guadalajara. M.A.G. and E.S. acknowledge financial support by grants AYA 2014-57280-P and PGC 2018-102184-B-I00, cofunded with FEDER funds. M.A.G. acknowledges support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). E.S. acknowledges the hospitality of the IAA during a short-term visit. G.R.L. acknowledges support from CONACyT and PRODEP (Mexico). L.S. acknowledges support from UNAM DGAPA PAPIIT project IN101819. M.A.G. and J.A.T. acknowledge support from the UNAM DGAPA PAPIIT project IA 100318. We appreciate the valuable comments of the referee, Dr Nye Evans. Finally, we thank Alessandro Ederoclite for useful discussions and comments. The data presented here were obtained in part with ALFOSC, and provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. This research made use of IRAF, distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. We acknowledge the use of the ESO Science Archive Facility developed in partnership with the Space Telescope European Coordinating Facility (ST-ECF). We also acknowledge the ING archive, maintained as part of the CASU Astronomical Data Centre at the Institute of Astronomy, Cambridge and finally, the STScI, operated by the Association of Universities for research in Astronomy, Inc., under NASA contract NAS5-26555.

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., Born-again stars allow probing stellar evolution in human timescales and provide the most promising path for the formation of hydrogen-deficient post-asymptotic giant branch objects, but their cold and molecular components remain poorly explored. Here we present ALMA observations of V 605 Aql that unveil for the first time the spatio-kinematic distribution of the molecular material associated with a born-again star. Both the continuum and molecular line emission exhibit a clumpy ring-like structure with a total extent of ≈1'' in diameter. The bulk of the molecular emission is interpreted as being produced in a radially expanding disk-like structure with an expansion velocity ${v}_{\exp }$ ∼ 90 km s−1 and an inclination i ≈ 60° with respect to the line of sight. The observations also reveal a compact high-velocity component, ${v}_{\exp }$ ∼ 280 km s−1, that is aligned perpendicularly to the expanding disk. This component is interpreted as a bipolar outflow with a kinematical age τ ≲ 20 yr, which could either be material that is currently being ejected from V 605 Aql, or is being dragged from the inner parts of the disk by a stellar wind. The dust mass of the disk is in the range Mdust ∼ 0.2–8 × 10−3 M⊙, depending on the dust absorption coefficient. The mass of the CO is MCO ≈ 1.1 × 10−5 M⊙, which is more than three orders of magnitude larger than the mass of the other detected molecules. We estimate a 12C/13C ratio of 5.6 ± 0.6, which is consistent with the single stellar evolution scenario in which the star experienced a very late thermal pulse instead of a nova-like event as previously suggested. © 2022. The Author(s). Published by the American Astronomical Society., This Letter makes use of the following ALMA data: ADS/ JAO.ALMA#2019.1.01408.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST, and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. J.A.T. is grateful for funding by Fundación Marcos Moshinsky (México) and the DGAPA UNAM projects IA100720 and IA101622. J.B.R.G. thanks Consejo Nacional de Ciencias y Tecnología (CONACYT) Mexico for a research student grant. M.A.G. acknowledges support from the Spanish Ministerio de Ciencia, Innovación y Universidades (MCIU) grant PGC2018-102184-B-I00 and from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). L.A.Z. acknowledges financial support from CONACyT-280775 and UNAM-PAPIIT IN110618 grants, México. S.P.T.M. acknowledges the Chalmers Gender Initiative for Excellence (Genie). This work has made extensive use of NASA's Astrophysics Data System. The authors thank Theo Khouri for helpful discussions. The authors also thank the anonymous referee for constructive comments and suggestions that helped to improve the manuscript.

We present the first part of an investigation on the planetary nebula (PN) PC 22 that focuseson the use of deep imaging and high-resolution echelle spectroscopy to perform a detailedmorpho-kinematical analysis. PC 22 is revealed to be a multipolar PN emitting predominantlyin [O III] and displaying multiple non-symmetric outflows. Its central region is found to be alsoparticularly inhomogeneous with a series of low-ionization structures (knots) located on thepath of the outflows. The morpho-kinematical model obtained with SHAPE indicates that (i) thede-projected velocities of the outflows are rather large, ≥100 km s, while the central regionhas expansion velocities in the range ∼25 to ∼45 km s following the 'Wilson effect'; (ii) themajority of the measured structures share similar inclination, ≃100°, i.e. they are coplanar;(iii) and all outflows and lobes are coeval (within the uncertainties). All these results make usto suggest that PC 22 is an evolved starfish PN.We propose that the mechanism responsible forthe morphology of PC 22 consists of a wind-shell interaction, where the fast post-asymptoticgiant branch (AGB) wind flows through a filamentary AGB shell with some large voids.© 2017 The Authors., LS acknowledges support from PAPIIT grant IA-101316 (Mexico). GR-L acknowledges support from CONACYT, CGCI, PRODEP and SEP (Mexico). MAG acknowledges support of the grant AYA 201457280-P, co-funded with FEDER funds. SZ acknowledges support from the UNAM-ITE collaboration agreement 1500-479-3-V-04.

A significant fraction of planetary nebulae (PNe) exhibit collimated outflows, distinct narrow kinematical components with notable velocity shifts with respect to the main nebular shells typically associated with low-ionization compact knots and linear or precessing jet-like features. We present here a spatio-kinematical investigation of a sample of 12 PNe with morphologies in emission lines of low-ionization species suggestive of collimated outflows. Using archival narrow-band images and our own high-dispersion long-slit echelle spectra, we confirm the presence of collimated outflows in Hen 2-429, J 320, M 1-66, M 2-40, M 3-1, and NGC 6210 and possibly in NGC 6741, for which the spatio-kinematical data can also be interpreted as a pair of bipolar lobes. The presence of collimated outflows is rejected in Hen 2-47, Hen 2-115, M 1-26, and M 1-37, but their morphology and kinematics are indicative of the action of supersonic outflows that have not been able to pierce through the nebular envelope. In this sense, M 1-66 appears to have experienced a similar interaction between the outflow and nebular envelope, but, as opposed to these four PNe, the outflow has been able to break through the nebular envelope. It is suggested that the PNe without collimated outflows in our sample are younger or descend from lower mass progenitors than those that exhibit unambiguous collimated outflows. © 2019 The Author(s), JSR-G and MAG acknowledge support of the grants AYA 2014-57280-P and PGC2018-102184-B-I00, co-funded with FEDER funds. SDP acknowledges financial support from the Spanish Ministerio de Econom?a y Competitividad under grants AYA2013 47742-C4-1-P and AYA2016 79724-C4-4-P, from Junta de Andaluc?a Excellence Project PEX2011 FQM-7058. JAT and MAG are also funded by UNAM DGAPA PAPIIT project IA100318. LFM acknowledges partial support by grant AYA2017-84390-C2-R, co-funded with FEDER funds. JSR-G, MAG, LFM, and SDP acknowledge financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrof?sica de Andaluc?a (SEV-2017-0709). We thank Dr. Laurence Sabin for a thorough reading of the manuscript and her valuable comments that helped us to improve it. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (STECF/ ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This research has made also use of the NASA's Astrophysics Data System. This research made use of PYTHON (http://www.python.o rg) and IPYTHON (P?rez, & Granger 2007), APLpy (Robitaille, & Bressert 2012), Numpy (Van Der Walt, Colbert & Varoquaux 2011), Pandas (McKinney 2010), and Matplotlib (Hunter 2007), a suite of open-source PYTHON modules that provides a framework for creating scientific plots. This research made use of Astropy, a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013). The Astropy web site is http://www.astropy.org.

We present a detailed comparative study of the arcs and fragmented ring-like features in the haloes of the planetary nebulae (PNe) NGC 6543, NGC 7009, and NGC 7027 and the spiral pattern around the carbon star AFGL 3068 using high-quality multi-epoch HST images. This comparison allows us to investigate the connection and possible evolution between the regular patterns surrounding AGB stars and the irregular concentric patterns around PNe. The radial proper motion of these features, ≃15 km s-1, are found to be consistent with the AGB wind and their linear sizes and inter-lapse times (500 - 1900 yr) also agree with those found around AGB stars, suggesting a common origin. We find evidence using radiative-hydrodynamic simulations that regular patterns produced at the end of the AGB phase become highly distorted by their interactions with the expanding PN and the anisotropic illumination and ionization patterns caused by shadow instabilities. These processes will disrupt the regular (mostly spiral) patterns around AGB stars, plausibly becoming the arcs and fragmented rings observed in the haloes of PNe.© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society, The authors acknowledge support from grants AYA 2014-57280- P and PGC2018-102184-B-I00, co-funded with FEDER funds. JAT and MAG are funded by DGAPA, UNAM PAPIIT project IA100318, and LS by DGAPA, UNAM PAPIIT project IN101819. GRL acknowledges support from Fundacion Marcos Moshinsky, ´ Consejo Nacional de Ciencia y Tecnolog´ıa (CONACyT), and Programa para el Desarrollo Profesional Docente (PRODEP) (Mexico). BB acknowledges support from program AR-14563 that was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This paper is based on observations made with the NASA/ESAHubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). The large scale image of NGC 7009 is based on observations collected at the European Southern Observatory by the MUSE science verification team. This work has made extensive use of the NASA’s Astrophysics Data System.

HuBi 1 has been proposed to be member of the rare class of born-again planetary nebulae (PNe), i.e., its central star experienced a very late thermal pulse and ejected highly processed material at high speeds inside the old hydrogen-rich PN. In this Letter we present GTC MEGARA integral field spectroscopic observations of the innermost regions of HuBi 1 at high spectral resolution ≃16 km s-1 and multi-epoch subarcsecond images obtained ≃12 yr apart. The analysis of these data indicates that the inner regions of HuBi 1 were ejected ≃200 yr ago and expand at velocities ≃300 km s-1, in excellent agreement with the born-again scenario. The unprecedented tomographic capabilities of the GTC MEGARA high-dispersion observations used here reveal that the ejecta in HuBi 1 has a shell-like structure, in contrast to the disrupted disk and jet morphology of the ejecta in other born-again PNe. © 2020. The American Astronomical Society. All rights reserved., J.S.R.G. and V.M.A.G.G. acknowledge support from the Programa de Becas posdoctorales of DGAPA UNAM (Mexico). J.S.R.G., V.M.A.G.G., and J.A.T. are funded by the UNAM DGAPA PAPIIT project IA100720 (Mexico). M.A. G. acknowledges support of the Spanish Ministerio de Ciencia, Innovacion y Universidades (MCIU) grant PGC2018-102184-B-I00. M.A.G., S.C., and L.F.M. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). E.S. and G.R.L. acknowledge support from CONACyT. (grant 263373). L.S. acknowledges support from PAPIIT-UNAM grant IN101819. L.F.M. is partially supported by MCIU grant AYA2017-84390-C2-1-R. J.S.R.G. and V.M.A.G.G. thank INAOE for its hospitality during a training course on reduction and analysis of MEGARA data and the organizers of this course Y. D. Mayya and J. Zaragoza-Cardiel for sharing their expertise with us. The GTC Science Operations team is acknowledged for scheduling the GTC MEGARA observations under the stringent conditions demanded by this program.

Fast highly collimated outflows, including bipolar knots, jetlike features, and point-symmetric filaments or strings of knots, are common in planetary nebulae (PNe). These features, generally known as jets, are thought to play an active role in the nebular shaping immediately before or while fast stellar winds and D-type ionization fronts shock and sweep up the nebular envelope. The space velocity, radial distance from the central star, and kinematic age of the jets in PNe cannot be determined because the inclination angle with the line of sight is usually unknown. Here we have used the large number of jets already detected in PNe to derive orientation-independent properties from a statistical point of view. We find that jets in PNe can be assigned to two different populations: most (about 70%) have space velocities below 100 km s-1, and only 30% have larger velocities. Since a significant fraction of jets move at velocities similar to that of their parent PNe and are found close to the nebular edge, we propose that these jets have been slowed down in their interaction with the nebular envelope, contributing to the expansion of their PNe. The time spans before the jets dissolve are found to be generally shorter than 2500 yr. Since most jets are found in young PNe of similar (1000-3000 yr) age, it can be concluded that jets are mostly coeval with their PNe. © 2020. The American Astronomical Society. All rights reserved.., The authors acknowledge support from grants AYA 201457280-P and PGC2018-102184-B-I00, cofunded with FEDER funds. J.S.R.G. acknowledges financial support from DGAPA-PAPIIT grants IN103117 (PI: Dr. Miriam Pena) and IG100218 (PI: Dr. Pablo F. Velazquez) and scholarship from BECA MIXTA CONACyT-Mexico. This research was motivated a long time ago during an inspiring coffee talk with Dr. Hugo Schwarz. The authors deeply appreciate Dr. Pablo F. Velazquez for his helpful comments, Dr. Jose A. Lopez for a thorough reading of the manuscript and providing us access to spatiokinematic data from the SPM Kinematic Catalogue of Galactic Planetary Nebulae, and Drs. Noam Soker and B. Balick for their many comments and contributions to the final version of this manuscript.

Nebular He ii emission implies the presence of energetic photons (E ≥ 54 eV). Despite the great deal of effort dedicated to understanding He ii ionization, its origin has remained mysterious, particularly in metal-deficient star-forming (SF) galaxies. Unfolding He ii-emitting, metal-poor starbursts at z ~ 0 can yield insight into the powerful ionization processes occurring in the primordial universe. Here we present a new study on the effects that X-ray sources have on the He ii ionization in the extremely metal-poor galaxy IZw18 (Z ~ 3% Z⊙), whose X-ray emission is dominated by a single high-mass X-ray binary (HMXB). This study uses optical integral field spectroscopy, archival Hubble Space Telescope observations, and all of the X-ray data sets publicly available for IZw18. We investigate the time-variability of the IZw18 HMXB for the first time; its emission shows small variations on timescales from days to decades. The best-fit models for the HMXB X-ray spectra cannot reproduce the observed He ii ionization budget of IZw18, nor can recent photoionization models that combine the spectra of both very low metallicity massive stars and the emission from HMXB. We also find that the IZw18 HMXB and the He ii-emission peak are spatially displaced at a projected distance of sime200 pc. These results reduce the relevance of X-ray photons as the dominant He ii ionizing mode in IZw18, which leaves uncertain what process is responsible for the bulk of its He ii ionization. This is in line with recent work discarding X-ray binaries as the main source responsible for He ii ionization in SF galaxies. © 2021. The American Astronomical Society. All rights reserved., This work has been partially funded by projects AYA2016-79724-C4-4-P and PID2019-107408GB-C44 from the Spanish PNAYA. C.K., M.A.G., and J.V.M. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). M.A.G. acknowledges support from MCIU grant PGC2018-102184-B-I00 cofunded with FEDER funds. G.R.-L. acknowledges support from CONACyT (grant 263373) and PRODEP (Mexico). This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC.

The fast stellar winds can blow bubbles in the circumstellar material ejected from previous phases of stellar evolution. These are found at different scales, from planetary nebulae (PNe) around stars evolving to the white dwarf stage, to Wolf-Rayet (WR) bubbles and up to large-scale bubbles around massive star clusters. In all cases, the fast stellar wind is shock-heated and a hot bubble is produced. Processes of mass evaporation and mixing of nebular material and heat conduction occurring at the mixing layer between the hot bubble and the optical nebula are key to determine the thermal structure of these bubbles and their evolution. In this contribution we review our current understanding of the X-ray observations of hot bubbles in PNe and present the first spatially-resolved study of a mixing layer in a PN.

We present deep optical spectroscopy of seven planetary nebulae (PNe) in the substructures of M31, three in the Northern Spur and four associated with the Giant Stream. The spectra were obtained with the OSIRIS spectrograph on the 10.4 m GTC. The detection of the [O iii] λ4363 auroral line in all PNe of our sample enables reliable abundance determinations. Our targets have low N/O (

While most of the low-mass stars stay hydrogen-rich on their surface throughout their evolution, a considerable fraction of white dwarfs as well as central stars of planetary nebulae have a hydrogen-deficient surface composition. The majority of these H-deficient central stars exhibit spectra very similar to massive Wolf-Rayet stars of the carbon sequence, i.e. with broad emission lines of carbon, helium, and oxygen. In analogy to the massive Wolf-Rayet stars, they are classified as [WC] stars. Their formation, which is relatively well understood, is thought to be the result of a (very) late thermal pulse of the helium burning shell. It is therefore surprising that some H-deficient central stars which have been found recently, e.g. IC 4663 and Abell 48, exhibit spectra that resemble those of the massive Wolf-Rayet stars of the nitrogen sequence, i.e. with strong emission lines of nitrogen instead of carbon. This new type of central stars is therefore labelled [WN]. We present spectral analyses of these objects and discuss the status of further candidates as well as the evolutionary status and origin of the [WN] stars., 4 pages, 2 figures, IAUS 323