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6. Complex Molecules in the L1157 Molecular Outflow

Author

Jes K. Jørgensen, Mario Tafalla, Héctor G. Arce, Rafael Bachiller, and J. Santiago-Garcia

Subjects
Physics, Star formation, Molecular cloud, Astrophysics (astro-ph), Galactic Center, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Mantle (geology), Free molecular flow, Space and Planetary Science, Molecule, Protostar, Outflow
Abstract

We report the detection of complex organic molecules in the young protostellar outflow L1157. We identify lines from HCOOCH3, CH3CN, HCOOH and C2H5OH at the position of the B1 shock in the blueshifted lobe, making it the first time that complex species have been detected towards a molecular outflow powered by a young low-mass protostar. The time scales associated with the warm outflow gas (< 2,000 yr) are too short for the complex molecules to have formed in the gas phase after the shock-induced sputtering of the grain mantles. It is more likely that the complex species formed in the surface of grains and were then ejected from the grain mantles by the shock. The formation of complex molecules in the grains of low-mass star forming regions must be relatively efficient, and our results show the importance of considering the impact of outflows when studying complex molecules around protostars. The relative abundance with respect to methanol of most of the detected complex molecules is similar to that of hot cores and molecular clouds in the galactic center region, which suggests that the mantle composition of the dust in the L1157 dark cloud is similar to dust in those regions., 8 pages, 2 tables, 2 figures

Published
2008

7. Anatomy of the internal bow shocks in the IRAS 04166+2706 protostellar jet

Author

Qizhou Zhang, Hsien Shang, J. Santiago-Garcia, M. Tafalla, Naomi Hirano, Yu-Nung Su, Doug Johnstone, Chin-Fei Lee, and Liang-Yao Wang

Subjects
Field (physics), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Submillimeter Array, 0103 physical sciences, Perpendicular, Astrophysics::Solar and Stellar Astrophysics, Protostar, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, radio lines: ISM, Jet (fluid), stars: formation, 010308 nuclear & particles physics, Astronomy and Astrophysics, ISM: individual objects: IRAS 04166+2706, Astrophysics - Astrophysics of Galaxies, ISM: molecules, Core (optical fiber), ISM: jets and outflows, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow
Abstract

$Aims.$ We study the relation between the jet and the outflow in the IRAS 04166+2706 protostar. This Taurus protostar drives a molecular jet that contains multiple emission peaks symmetrically located from the central source. The protostar also drives a wide-angle outflow consisting of two conical shells. $Methods.$ We have used the Atacama Large Millimeter/submillimeter Array (ALMA) interferometer to observe two fields along the IRAS 04166+2706 jet. The fields were centered on a pair of emission peaks that correspond to the same ejection event, and were observed in CO(2-1), SiO(5-4), and SO(65-54). $ Results.$ Both ALMA fields present spatial distributions that are approximately elliptical and have their minor axes aligned with the jet direction. As the velocity increases, the emission in each field moves gradually across the elliptical region. This systematic pattern indicates that the emitting gas in each field lies in a disk-like structure that is perpendicular to the jet axis and is expanding away from the jet. A small degree of curvature in the first-moment maps indicates that the disks are slightly curved in the manner expected for bow shocks moving away from the IRAS source. A simple geometrical model confirms that this scenario fits the main emission features. $Conclusions.$ The emission peaks in the IRAS 04166+2706 jet likely represent internal bow shocks where material is being ejected laterally away from the jet axis. While the linear momentum of the ejected gas is dominated by the component in the jet direction, the sideways component is not negligible, and can potentially affect the distribution of gas in the surrounding outflow and core., Comment: 12 pages, 12 figures, accepted for publication in A&A

Published
2017

8. High-pressure, low-abundance water in bipolar outflows. Results from a Herschel-WISH survey

Author

M. Tafalla, René Liseau, Rafael Bachiller, Lars E. Kristensen, J. Santiago-Garcia, Brunella Nisini, Gregory J. Herczeg, Umut A. Yildiz, and E. F. van Dishoeck

Subjects
Physics, 010504 meteorology & atmospheric sciences, Kelvin, Young stellar object, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spatial distribution, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, 6. Clean water, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Thermal, Radiative transfer, Outflow, Low Mass, 010303 astronomy & astrophysics, Intensity (heat transfer), 0105 earth and related environmental sciences
Abstract

(Abridged) We present a survey of the water emission in a sample of more than 20 outflows from low mass young stellar objects with the goal of characterizing the physical and chemical conditions of the emitting gas. We have used the HIFI and PACS instruments on board the Herschel Space Observatory to observe the two fundamental lines of ortho-water at 557 and 1670 GHz. These observations were part of the "Water In Star-forming regions with Herschel" (WISH) key program, and have been complemented with CO and H2 data. We find that the emission from water has a different spatial and velocity distribution from that of the J=1-0 and 2-1 transitions of CO, but it has a similar spatial distribution to H2, and its intensity follows the H2 intensity derived from IRAC images. This suggests that water traces the outflow gas at hundreds of kelvins responsible for the H2 emission, and not the component at tens of kelvins typical of low-J CO emission. A warm origin of the water emission is confirmed by a remarkable correlation between the intensities of the 557 and 1670 GHz lines, which also indicates the emitting gas has a narrow range of excitations. A non-LTE radiative transfer analysis shows that while there is some ambiguity on the exact combination of density and temperature values, the gas thermal pressure nT is constrained within less than a factor of 2. The typical nT over the sample is 4 10^{9} cm^{-3}K, which represents an increase of 10^4 with respect to the ambient value. The data also constrain within a factor of 2 the water column density. When this quantity is combined with H2 column densities, the typical water abundance is only 3 10^{-7}, with an uncertainty of a factor of 3. Our data challenge current C-shock models of water production due to a combination of wing-line profiles, high gas compressions, and low abundances., 21 pages, 13 figures. Accepted for publication in A&A

Published
2013

9. Molecular Jet of IRAS 04166+2706

Author

Mario Tafalla, Hsien Shang, Chin-Fei Lee, Naomi Hirano, Yu-Nung Su, J. Santiago-Garcia, Qizhou Zhang, and Liang-Yao Wang

Subjects
Physics, Mean kinetic temperature, Velocity gradient, Plateau de Bure Interferometer, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Submillimeter Array, Astrophysics - Astrophysics of Galaxies, Stars, Knot (unit), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astronomical interferometer, Outflow, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The molecular outflow from IRAS 04166+2706 was mapped with the Submillimeter Array (SMA) at 350 GHz continuum and CO J = 3$-$2 at an angular resolution of ~1 arcsec. The field of view covers the central arc-minute, which contains the inner four pairs of knots of the molecular jet. On the channel map, conical structures are clearly present in the low velocity range (|V$-$V$_0$|$$|V$-$V$_0$|$>$30 km s$^{-1}$). The higher angular resolution of ~1 arcsec reveals the first blue-shifted knot (B1) that was missing in previous PdBI observation of Sant\'iago-Garc\'ia et al. (2009) at an offset of ~6 arcsec to the North-East of the central source. This identification completes the symmetric sequence of knots in both the blue- and red-shifted lobes of the outflow. The innermost knots R1 and B1 have the highest velocities within the sequence. Although the general features appear to be similar to previous CO J = 2$-$1 images in Sant\'iago-Garc\'ia et al. (2009), the emission in CO J = 3$-$2 almost always peaks further away from the central source than that of CO J = 2$-$1 in the red-shifted lobe of the channel maps. This gives rise to a gradient in the line-ratio map of CO J = 3$-$2/J = 2$-$1 from head to tail within a knot. A large velocity gradient (LVG) analysis suggests that the differences may reflect a higher gas kinetic temperature at the head. We also explore possible constraints imposed by the non-detection of SiO J = 8$-$7., Comment: 32 pages, 12 figures, 1 table, accepted for publication in ApJ

Published
2013
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10. Herschel/HIFI detections of hydrides towards AFGL 2591. Envelope emission versus tenuous cloud absorption [Letter]

Author

Javier R. Goicoechea, M. Tafalla, Pierre Encrenaz, P. Stäuber, Jes K. Jørgensen, Jonathan Braine, T. Giannini, Laurent Pagani, Steven D. Doty, Alain Baudry, Michael Olberg, Rafael Bachiller, M. Marseille, Th. de Graauw, E. F. van Dishoeck, Lars E. Kristensen, R. Schieder, José Cernicharo, André Csillaghy, S. Bruderer, S. F. Wampfler, T. A. van Kempen, Paolo Saraceno, Arnold O. Benz, Gary J. Melnick, David A. Neufeld, T. Jacq, C. Dedes, J. Santiago-Garcia, N. Honingh, John C. Pearson, R. Shipman, Frank Helmich, D. Teyssier, M. Fich, A. Di Giorgio, Willem Jellema, Edwin Bergin, Per Bjerkeli, N. Whyborn, Paola Caselli, R. Plume, Ruud Visser, Dariusz C. Lis, M. Melchior, Fabrice Herpin, Christophe Risacher, B. Larsson, Emmanuel Caux, Brunella Nisini, C. McCoey, Christian Monstein, F. Daniel, Geoffrey A. Blake, Doug Johnstone, Gregory J. Herczeg, Umut A. Yildiz, Berengere Parise, Claudio Codella, Sylvain Bontemps, René Liseau, Milena Benedettini, Michiel R. Hogerheijde, Friedrich Wyrowski, Carsten Dominik, F. F. S. van der Tak, W. Bächtold, Asunción Fuente, Low Energy Astrophysics (API, FNWI), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), SRON Netherlands Institute for Space Research (SRON), INAF - Osservatorio Astronomico di Roma (OAR), Onsala Space Observatory, Chalmers University of Technology [Göteborg], ESO, European Southern Observatory (ESO), Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Radioastronomie (MPIFR), École normale supérieure - Paris (ENS Paris), European Space Agency (ESA)-European Space Agency (ESA), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, and Consiglio Nazionale delle Ricerche (CNR)

Subjects
Photon, FOS: Physical sciences, Astrophysics, 7. Clean energy, Far infrared, CHEMISTRY, EXCITATION, OUTFLOW, Solar and Stellar Astrophysics, Spectral resolution, H2O+, Absorption (electromagnetic radiation), Solar and Stellar Astrophysics (astro-ph.SR), Envelope (waves), QB, STAR-FORMING REGIONS, Physics, stars: formation, SPECTROSCOPY, INTERSTELLAR-MEDIUM, astrochemistry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Diatomic molecule, ISM: molecules, Astrophysics - Solar and Stellar Astrophysics, GL-2591, 13. Climate action, Space and Planetary Science, ABUNDANCE, Outflow, ISM: individual objects: AFGL 2591, Excitation
Abstract

The Heterodyne Instrument for the Far Infrared (HIFI) onboard the Herschel Space Observatory allows the first observations of light diatomic molecules at high spectral resolution and in multiple transitions. Here, we report deep integrations using HIFI in different lines of hydrides towards the high-mass star forming region AFGL 2591. Detected are CH, CH+, NH, OH+, H2O+, while NH+ and SH+ have not been detected. All molecules except for CH and CH+ are seen in absorption with low excitation temperatures and at velocities different from the systemic velocity of the protostellar envelope. Surprisingly, the CH(JF,P = 3/2_2,- - 1/2_1,+) and CH+(J = 1 - 0, J = 2 - 1) lines are detected in emission at the systemic velocity. We can assign the absorption features to a foreground cloud and an outflow lobe, while the CH and CH+ emission stems from the envelope. The observed abundance and excitation of CH and CH+ can be explained in the scenario of FUV irradiated outflow walls, where a cavity etched out by the outflow allows protostellar FUV photons to irradiate and heat the envelope at larger distances driving the chemical reactions that produce these molecules., Comment: Accepted for publication in Astronomy and Astrophysics (HIFI first results issue)

Published
2010

11. Sensitive limits on the abundance of cold water vapor in the DM Tau protoplanetary disk

Author

T. A. Bell, Per Bjerkeli, A. Baudry, E. F. van Dishoeck, Friedrich Wyrowski, J. Santiago-Garcia, Jeffrey K. J. Fogel, Christian Brinch, D. Johnstone, Rene Plume, Fabien Daniel, Christophe Risacher, S. Bruderer, David A. Neufeld, Steven D. Doty, R. Shipman, J. Stutzki, Paola Caselli, Olja Panić, G. J. Herczeg, A. Fuente, Aggm Tielens, J. R. Goicoechea, Michael Olberg, G. A. Blake, C. Codella, E. A. Bergin, M. Fich, Bengt Larsson, Th. de Graauw, Berengere Parise, René Liseau, Rafael Bachiller, M. Benedettini, Paul Hartogh, Brunella Nisini, J. C. Pearson, Ryszard Szczerba, Mario Tafalla, Jes K. Jørgensen, F. F. S. van der Tak, Umut A. Yildiz, Michiel R. Hogerheijde, T. A. van Kempen, M. Marseille, Carsten Dominik, Frank Helmich, J. Braine, P. J. Encrenaz, Arnold O. Benz, Sylvain Bontemps, Susanne F. Wampfler, Fabrice Herpin, C. McCoey, P. Saraceno, Lars E. Kristensen, R. Visser, Teresa Giannini, José Cernicharo, T. Jacq, Willem Jellema, Gary J. Melnick, A. M. di Giorgio, Dariusz C. Lis, Low Energy Astrophysics (API, FNWI), Astronomy, Kapteyn Astronomical Institute, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Civilisations atlantiques & Archéosciences (C2A), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Ministère de la Culture et de la Communication (MCC)-Université de Rennes 2 (UR2), Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)-Université de Nantes - UFR Histoire, Histoire de l'Art et Archéologie (UFR HHAA), Université de Nantes (UN)-Université de Nantes (UN), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), INAF - Osservatorio Astronomico di Roma (OAR), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, ESO, European Southern Observatory (ESO), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Radioastronomie (MPIFR), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Harvard University-Smithsonian Institution, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), École normale supérieure - Paris (ENS-PSL), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Smithsonian Institution-Harvard University [Cambridge], Université de Nantes - UFR Histoire, Histoire de l'Art et Archéologie (UFR HHAA), and Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Ministère de la Culture et de la Communication (MCC)

Subjects
DESORPTION, Abundance (chemistry), [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, DUST, Astrophysics, Protoplanetary disk, 01 natural sciences, ISM: abundances, MOLECULES, PLANET-FORMING REGION, CIRCUMSTELLAR DISKS, 0103 physical sciences, H2O, SPECTRA, Solar and Stellar Astrophysics, Emission spectrum, 010306 general physics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Line (formation), Physics, Earth and Planetary Astrophysics (astro-ph.EP), Spectrometer, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, protoplanetary disks, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ISM: molecules, EVOLUTION, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, GAS, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Earth and Planetary Astrophysics, Water ice, Water vapor, Intensity (heat transfer), STARS, Astrophysics - Earth and Planetary Astrophysics
Abstract

We performed a sensitive search for the ground-state emission lines of ortho- and para-water vapor in the DM Tau protoplanetary disk using the Herschel/HIFI instrument. No strong lines are detected down to 3sigma levels in 0.5 km/s channels of 4.2 mK for the 1_{10}--1_{01} line and 12.6 mK for the 1_{11}--0_{00} line. We report a very tentative detection, however, of the 1_{10}--1_{01} line in the Wide Band Spectrometer, with a strength of T_{mb}=2.7 mK, a width of 5.6 km/s and an integrated intensity of 16.0 mK km/s. The latter constitutes a 6sigma detection. Regardless of the reality of this tentative detection, model calculations indicate that our sensitive limits on the line strengths preclude efficient desorption of water in the UV illuminated regions of the disk. We hypothesize that more than 95-99% of the water ice is locked up in coagulated grains that have settled to the midplane., 5 pages, 3 figures. Accepted for publication in the Herschel HIFI special issue of A&A

Published
2010

12. Herschel/HIFI observations of high-J CO lines in the NGC 1333 low-mass star-forming region

Author

Fabrice Herpin, José Cernicharo, Carsten Dominik, A. Di Giorgio, T. Jacq, Pierre Encrenaz, Doug Johnstone, Claudio Codella, Steven D. Doty, M. Fich, F. F. S. van der Tak, Jes K. Jørgensen, Gregory J. Herczeg, Volker Ossenkopf, Paola Caselli, S. F. Wampfler, M. Marseille, Edwin Bergin, Per Bjerkeli, T. A. van Kempen, Michiel R. Hogerheijde, Sylvain Bontemps, Jonathan Braine, Alain Baudry, Asunción Fuente, Juergen Stutzki, J. Santiago-Garcia, E. Deul, Ruud Visser, Willem Jellema, René Liseau, Javier R. Goicoechea, Paolo Saraceno, Christophe Risacher, Umut A. Yildiz, David A. Neufeld, Berengere Parise, Milena Benedettini, Pieter Dieleman, Frank Helmich, E. F. van Dishoeck, R. Schieder, John C. Pearson, Dariusz C. Lis, Lars E. Kristensen, F.-C. Liu, T. Giannini, Arnold O. Benz, F. Daniel, Friedrich Wyrowski, Rafael Bachiller, Geoffrey A. Blake, Russel Shipman, Alexander G. G. M. Tielens, Th. de Graauw, Michael Olberg, Gary J. Melnick, C. McCoey, B. Larsson, Brunella Nisini, R. Plume, M. Tafalla, Simon Bruderer, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), INAF - Osservatorio Astronomico di Roma (OAR), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, ESO, European Southern Observatory (ESO), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Radioastronomie (MPIFR), Astronomy, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), École normale supérieure - Paris (ENS-PSL), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), and Low Energy Astrophysics (API, FNWI)

Subjects
010504 meteorology & atmospheric sciences, Astronomy, Evaporation, FOS: Physical sciences, DUST, Astrophysics, Star (graph theory), 01 natural sciences, DENSE CORES, 0103 physical sciences, Radiative transfer, Protostar, WATER, Solar and Stellar Astrophysics, Isotopologue, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QB, 0105 earth and related environmental sciences, Envelope (waves), Line (formation), Physics, stars: formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], astrochemistry, NGC-1333 IRAS-4, PROTOSTARS, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], H2CO, ISM: molecules, EVOLUTION, ENVELOPES, ISM: jets and outflows, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, ABUNDANCE, Low Mass, HIFI
Abstract

Herschel-HIFI observations of high-J lines (up to J_u=10) of 12CO, 13CO and C18O are presented toward three deeply embedded low-mass protostars, NGC 1333 IRAS 2A, IRAS 4A, and IRAS 4B, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. The spectrally-resolved HIFI data are complemented by ground-based observations of lower-J CO and isotopologue lines. The 12CO 10-9 profiles are dominated by broad (FWHM 25-30 km s^-1) emission. Radiative transfer models are used to constrain the temperature of this shocked gas to 100-200 K. Several CO and 13CO line profiles also reveal a medium-broad component (FWHM 5-10 km s^-1), seen prominently in H2O lines. Column densities for both components are presented, providing a reference for determining abundances of other molecules in the same gas. The narrow C18O 9-8 lines probe the warmer part of the quiescent envelope. Their intensities require a jump in the CO abundance at an evaporation temperature around 25 K, thus providing new direct evidence for a CO ice evaporation zone around low-mass protostars., Comment: 8 pages, 9 figures

Published
2010

13. Water in low-mass star-forming regions with Herschel . HIFI spectroscopy of NGC 1333

Author

Rafael Bachiller, Christophe Risacher, N. Whyborn, Steven D. Doty, A. Baudry, Per Bjerkeli, David A. Neufeld, Rene Plume, R. Shipman, F.-C. Liu, Pieter Dieleman, Sylvain Bontemps, Fabrice Herpin, E. F. van Dishoeck, M. Benedettini, Pieter R. Roelfsema, C. McCoey, José Cernicharo, Paola Caselli, J. Stutzki, Carsten Dominik, Paolo Saraceno, J. Braine, R. Visser, M. Fich, Susanne F. Wampfler, Frank Helmich, C. Codella, A. de Jonge, A. M. di Giorgio, Lars E. Kristensen, Friedrich Wyrowski, Geoffrey A. Blake, Teresa Giannini, E. Deul, Dariusz C. Lis, F. F. S. van der Tak, Volker Ossenkopf, J. Santiago-Garcia, Christian Brinch, M. Marseille, Th. de Graauw, Bengt Larsson, T. Jacq, Umut A. Yildiz, Mario Tafalla, A. Fuente, Jes K. Jørgensen, Arnold O. Benz, Fabien Daniel, Gary J. Melnick, S. Bruderer, Berengere Parise, Brunella Nisini, P. J. Encrenaz, Michiel R. Hogerheijde, T. A. van Kempen, René Liseau, D. A. Beintema, D. Johnstone, Aggm Tielens, J. R. Goicoechea, Michael Olberg, Michael J. Kaufman, J. C. Pearson, G. J. Herczeg, E. A. Bergin, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), INAF - Osservatorio Astronomico di Roma (OAR), Onsala Space Observatory, Chalmers University of Technology [Göteborg], ESO, European Southern Observatory (ESO), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Radioastronomie (MPIFR), Astronomy, Low Energy Astrophysics (API, FNWI), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Harvard University-Smithsonian Institution, École normale supérieure - Paris (ENS-PSL), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)

Subjects
010504 meteorology & atmospheric sciences, Astronomy, Young stellar object, FOS: Physical sciences, PROTOSTELLAR ENVELOPES, Astrophysics, PHYSICAL STRUCTURE, 01 natural sciences, DISK, Abundance (ecology), 0103 physical sciences, Protostar, OUTFLOW, Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Envelope (waves), Line (formation), QB, Physics, stars: formation, astrochemistry, Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], NGC-1333 IRAS-4, PROTOSTARS, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ISM: molecules, ISM: jets and outflows, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, VAPOR, ABUNDANCE, Outflow, SUBMILLIMETER, EMISSION, Low Mass, ISM: individual objects: NGC 1333
Abstract

'Water In Star-forming regions with Herschel' (WISH) is a key programme dedicated to studying the role of water and related species during the star-formation process and constraining the physical and chemical properties of young stellar objects. The Heterodyne Instrument for the Far-Infrared (HIFI) on the Herschel Space Observatory observed three deeply embedded protostars in the low-mass star-forming region NGC1333 in several H2-16O, H2-18O, and CO transitions. Line profiles are resolved for five H16O transitions in each source, revealing them to be surprisingly complex. The line profiles are decomposed into broad (>20 km/s), medium-broad (~5-10 km/s), and narrow (20 km/s), indicating that its physical origin is the same as for the broad H2-16O component. In one of the sources, IRAS4A, an inverse P Cygni profile is observed, a clear sign of infall in the envelope. From the line profiles alone, it is clear that the bulk of emission arises from shocks, both on small (, Accepted for publication in the A&A HIFI special issue

Published
2010

14. A molecular survey of outflow gas: velocity-dependent shock chemistry and the peculiar composition of the EHV gas

Author

M. Tafalla, Alvaro Hacar, J. Santiago-Garcia, and Rafael Bachiller

Subjects
Physics, Wing, Molecular composition, Shock (fluid dynamics), Gas velocity, High velocity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Spectral line, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Protostar, Outflow
Abstract

(Abridged) We present a molecular survey of the outflows powered by L1448-mm and IRAS 04166+2706, two sources with prominent wing and extremely high velocity (EHV) components in their CO spectra. The molecular composition of the two outflows presents systematic changes with velocity that we analyze by dividing the outflow in three chemical regimes, two of them associated with the wing component and the other the EHV gas. The analysis of the two wing regimes shows that species like H2CO and CH3OH favor the low-velocity gas, while SiO and HCN are more abundant in the fastest gas. We also find that the EHV regime is relatively rich in O-bearing species, as is not only detected in CO and SiO (already reported elsewhere), but also in SO, CH3OH, and H2CO (newly reported here), with a tentative detection in HCO+. At the same time, the EHV regime is relatively poor in C-bearing molecules like CS and HCN. We suggest that this difference in composition arises from a lower C/O ratio in the EHV gas. The different chemical compositions of the wing and EHV regimes suggest that these two outflow components have different physical origins. The wing component is better explained by shocked ambient gas, although none of the existing shock models explains all observed features. The peculiar composition of the EHV gas may reflect its origin as a dense wind from the protostar or its surrounding disk., Comment: 20 pages, 14 figures. Accepted by Astronomy and Astrophysics

Published
2010
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15. Origin of the hot gas in low-mass protostars: Herschel-PACS spectroscopy of HH 46

Author

T. Giannini, Patrick W. Morris, R. Shipman, Javier R. Goicoechea, A. Di Giorgio, Michael J. Kaufman, S. F. Wampfler, Sylvain Bontemps, René Liseau, Simon Bruderer, Ruud Visser, Fabrice Herpin, Mario Tafalla, R. H. Lin, Rafael Bachiller, F. F. S. van der Tak, Rene Plume, P. Saraceno, Christophe Risacher, Michel Fich, M. Marseille, Asunción Fuente, Arnold O. Benz, T. Jacq, Pierre Encrenaz, Th. de Graauw, Gregory J. Herczeg, T. A. van Kempen, Jes K. Jørgensen, Steven D. Doty, John C. Pearson, John Anthony Murphy, Jonathan Braine, E. F. van Dishoeck, Umut A. Yildiz, Neil Trappe, Doug Johnstone, Berengere Parise, Edwin Bergin, Per Bjerkeli, G. Melnick, S. Glenz, M. Benedettini, Christian Brinch, C. McCoey, Frank Helmich, R. Huisman, M. Ciechanowicz, F. Daniel, B. Larsson, Friedrich Wyrowski, Geoffrey A. Blake, Brunella Nisini, José Cernicharo, Alain Baudry, David A. Neufeld, Dariusz C. Lis, Michael Olberg, L. Dubbeldam, Lars E. Kristensen, J. Santiago-Garcia, Claudio Codella, Carsten Dominik, Paola Caselli, Michiel R. Hogerheijde, Low Energy Astrophysics (API, FNWI), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), INAF - Osservatorio Astronomico di Roma (OAR), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, ESO, European Southern Observatory (ESO), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Radioastronomie (MPIFR), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Harvard University-Smithsonian Institution, École normale supérieure - Paris (ENS-PSL), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), and Kapteyn Astronomical Institute

Subjects
Experimental Physics, Young stellar object, FOS: Physical sciences, Astrophysics, I, 01 natural sciences, Luminosity, 0103 physical sciences, Protostar, WATER, Solar and Stellar Astrophysics, OUTFLOW, 14. Life underwater, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Line (formation), Envelope (waves), QB, Physics, stars: formation, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], astrochemistry, Astronomy and Astrophysics, HH-46/47, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ISM: molecules, ISM: jets and outflows, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, ISM: individual objects: HH 46, JETS, SHOCK, Outflow, Low Mass, EMISSION
Abstract

'Water in Star-forming regions with Herschel' (WISH) is a Herschel Key Programme aimed at understanding the physical and chemical structure of young stellar objects (YSOs) with a focus on water and related species. The low-mass protostar HH 46 was observed with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory to measure emission in H2O, CO, OH, [OI], and [CII] lines located between 63 and 186 um. The excitation and spatial distribution of emission can disentangle the different heating mechanisms of YSOs, with better spatial resolution and sensitivity than previously possible. Far-IR line emission is detected at the position of the protostar and along the outflow axis. The OH emission is concentrated at the central position, CO emission is bright at the central position and along the outflow, and H2O emission is concentrated in the outflow. In addition, [OI] emission is seen in low-velocity gas, assumed to be related to the envelope, and is also seen shifted up to 170 km/s in both the red- and blue-shifted jets. Envelope models are constructed based on previous observational constraints. They indicate that passive heating of a spherical envelope by the protostellar luminosity cannot explain the high-excitation molecular gas detected with PACS, including CO lines with upper levels at >2500 K above the ground state. Instead, warm CO and H2O emission is probably produced in the walls of an outflow-carved cavity in the envelope, which are heated by UV photons and non-dissociative C-type shocks. The bright OH and [OI] emission is attributed to J-type shocks in dense gas close to the protostar. In the scenario described here, the combined cooling by far-IR lines within the central spatial pixel is estimated to be 2 \times 10-2 L_sun, with 60-80% attributed to J- and C-type shocks produced by interactions between the jet and the envelope., Accepted for publication in Astronomy and Astrophysics (Herschel special issue)

Published
2010

16. The extremely collimated bipolar H_2O jet from the NGC 1333-IRAS 4B protostar

Author

Mario Tafalla, J. F. Desmurs, Rafael Bachiller, Claudio Codella, and J. Santiago-Garcia

Subjects
Physics, Jet (fluid), Proper motion, Star formation, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, law.invention, Free molecular flow, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Protostar, Astrophysics::Solar and Stellar Astrophysics, Maser, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

We have performed observations of water maser emission towards a sample of low-mass protostars, in order to investigate the properties of jets associated with the earliest stages of star formation and their interaction with the surrounding medium. The main aim is to measure the absolute positions and proper motions of the H_2O spots in order to investigate the kinematics of the region from where the jet is launched. We imaged the protostars in the nearby region NGC 1333-IRAS 4 in the water maser line at 22.2 GHz by using the VLBA in phase-reference mode at the milliarcsecond scale over four epochs, spaced by one month to measure proper motions. Two protostars (A2 and B) were detected in a highly variable H_2O maser emission, with an active phase shorter than four weeks. The H_2O maps allow us to trace the fast jet driven by the B protostar: we observed both the red- and blue-shifted lobes very close to the protostar, =< 35 AU, moving away with projected velocities of ~10-50 km/s. The comparison with the molecular outflow observed at larger scale suggests a jet precession with a 18'/yr rate. By measuring the positional spread of the H_2O spots we estimate a jet width of ~2 AU at a distance of ~12 AU from the driving protostar., 9 pages, 8 figures, A&A accepted

Published
2009
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17. Shells, jets, and internal working surfaces in the molecular outflow from IRAS 04166+2706

Author

J. Santiago-Garcia, Rafael Bachiller, Doug Johnstone, and M. Tafalla

Subjects
Physics, Jet (fluid), Young stellar object, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Plateau de Bure Interferometer, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Collimated light, Interferometry, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Vector field, Outflow, Astrophysics::Galaxy Astrophysics
Abstract

Context: IRAS 04166+2706 in Taurus is one of the most nearby young stellar objects whose molecular outflow contains a highly collimated fast component. Methods: We have observed the IRAS 04166+2706 outflow with the IRAM Plateau de Bure interferometer in CO(J=2-1) and SiO(J=2-1) achieving angular resolutions between 2'' and 4''. To improve the quality of the CO(2-1) images, we have added single dish data to the interferometer visibilities. Results: The outflow consists of two distinct components. At velocities 30 km/s, the gas forms two opposed jets that travel along the center of the cavities and whose emission is dominated by a symmetric collection of at least 7 pairs of peaks. The velocity field of this component presents a sawtooth pattern with the gas in the tail of each peak moving faster than the gas in the head. This pattern, together with a systematic widening of the peaks with distance to the central source, is consistent with the emission arising from internal working surfaces traveling along the jet and resulting from variations in the velocity field of ejection. We interpret this component as the true protostellar wind, and we find its composition consistent with a chemical model of such type of wind. Conclusions: Our results support outflow wind models that have simultaneously wide-angle and narrow components, and suggest that the EHV peaks seen in a number of outflows consist of internally-shocked wind material., 13 pages, 10 figures. To appear in A&A

Published
2008
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19. Warm SiO gas in molecular bullets associated with protostellar outflows

Author

J. S. Richer, Rafael Bachiller, T. Giannini, J. Santiago Garcia, Claudio Codella, Brunella Nisini, and M. Tafalla

Subjects
Physics, Shock (fluid dynamics), High velocity, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Wavelength, Space and Planetary Science, Protostar, Millimeter, Excitation, Line (formation)
Abstract

In this paper we present the first SiO multiline analysis (from J=2-1 to J=11-10) of the molecular bullets along the outflows of the Class 0 sources L1448-mm and L1157-mm, obtained through observations with IRAM and JCMT. We have computed the main physical parameters in each bullet and compared them with other tracers of warm and dense gas and with models for the SiO excitation in shocks. We find that the bullets close to L1448--mm, associated with high velocity gas, have higher excitation conditions (n(H2) ~ 10^{6} cm^{-3}, T > 500 K) with respect to the L1157 bullets (n(H2) ~1-5 10^{5} cm^{-3}, T ~ 100-300 K). In both the sources, there is a clear evidence of the presence of velocity components having different excitation conditions, with the denser and/or warmer gas associated with the gas at the higher speed. In L1448 the bulk of the emission is due to the high-excitation and high velocity gas, while in L1157 most of the emission comes from the low excitation gas at ambient velocity. The observed velocity-averaged line ratios are well reproduced by shocks with speeds v_s larger than ~ 30 km/s and densities ~ 10^{5} - 10^{6} cm^{-3}. Plane-parallel shock models, however, fail to predict all the observed line profiles and in particular the very similar profiles shown by both low and high excitation lines. The overall observations support the idea that the L1157 clumps are shock interaction events older than the L1448 bullets close to the driving source. In the latter objects, the velocity structure and the variations of physical parameters with the velocity resemble very closely those found in optical/IR jets near the protostar, suggesting that similar launching and excitation mechanisms are also at the origin of collimated jets seen at millimetre wavelengths., 11pages, 9 figures, A&A accepted

Published
2006

20. A dinucleotide deletion in amyloid precursor protein (APP) mRNA associated with sporadic Alzheimer's disease results in efficient secretion of truncated APP isoforms from neuroblastoma cell cultures

Author

M, Hersberger, J, Santiago-Garcia, S, Patarroyo-White, J, Yan, and X, Xu

Subjects
DNA, Complementary, Recombinant Fusion Proteins, Green Fluorescent Proteins, Transfection, Rats, Molecular Weight, Amyloid beta-Protein Precursor, Luminescent Proteins, Neuroblastoma, Alzheimer Disease, Tumor Cells, Cultured, Animals, Humans, Protein Isoforms, RNA, Messenger, Sequence Deletion, Subcellular Fractions
Abstract

Recently, two dinucleotide deletions were detected in the mRNA of the amyloid precursor protein (APP) from cerebral cortex neurons of patients with sporadic Alzheimer's disease (AD) or Down's syndrome. These deletions resulted in truncation of APP, producing an APP isoform with a 38-kDa N-terminus and a novel carboxyl terminus (APP+1). We investigated the subcellular localization and the processing of APP+1 in the neuroblastoma cell line B103. cDNA constructs were generated encoding fusion proteins of APP+1 or full-length APP with the enhanced green fluorescent protein (eGFP). In transient transfection experiments using B103 cells, the APP+1-eGFP fusion protein showed a reticular localization with intense staining in the Golgi complex. Unlike full-length APP fused to eGFP, the APP+1-eGFP fusion protein did not localize to the perinuclear area or to the plasma membrane. Western blot analysis of cell extracts confirmed the translation of the expected fusion proteins. Analysis of the supernatant by western blot indicated that the APP+1-eGFP fusion protein was efficiently secreted from B103 cells, whereas the secreted form of full-length APP fusion protein (APPs) was hardly detectable. Thus, both dinucleotide deletions in the APP mRNA result in truncated APP+1 that is not membrane associated and is readily secreted from neurons.

Published
2001

21. Water vapor toward starless cores: The Herschel view

Author

Doug Johnstone, Steven D. Doty, Per Bjerkeli, Pierre Encrenaz, Dominicus Kester, F. Daniel, Jes K. Jørgensen, F. F. S. van der Tak, M. Marseille, Asunción Fuente, Geoffrey A. Blake, Christophe Risacher, A. Megej, Hamid Javadi, Javier R. Goicoechea, Jonathan Braine, J. Santiago-Garcia, John C. Pearson, Fabrice Herpin, Dariusz C. Lis, Arnold O. Benz, T. A. van Kempen, David A. Neufeld, Carsten Dominik, P. Siegel, T. Jacq, Simon Bruderer, Gregory J. Herczeg, T. Giannini, Umut A. Yildiz, Berengere Parise, Michiel R. Hogerheijde, Friedrich Wyrowski, E. F. van Dishoeck, P. Saraceno, Th. de Graauw, W. Luinge, Eric Keto, Sylvain Bontemps, René Liseau, José Cernicharo, A. Di Giorgio, Milena Benedettini, C. Codella, Ruud Visser, Lars E. Kristensen, C. McCoey, B. Larsson, Rafael Bachiller, Russel Shipman, Brunella Nisini, Brian Jackson, Gary J. Melnick, Alain Baudry, S. F. Wampfler, M. Tafalla, Paola Caselli, W. M. Laauwen, Todd Gaier, M. Fich, Edwin A. Bergin, Yuri Aikawa, R. Plume, Laurent Pagani, Michael Olberg, Frank Helmich, Kapteyn Astronomical Institute, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], INAF - Osservatorio Astronomico di Roma (OAR), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), SRON Netherlands Institute for Space Research (SRON), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, ESO, European Southern Observatory (ESO), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Radioastronomie (MPIFR), Low Energy Astrophysics (API, FNWI), École normale supérieure - Paris (ENS-PSL), Harvard University-Smithsonian Institution, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)

Subjects
Astronomy, FOS: Physical sciences, Astrophysics, INITIAL CONDITIONS, 7. Clean energy, ISM: clouds, OXYGEN, Gas phase, PRESTELLAR CORES, Radiative transfer, TEMPERATURE, Physics, stars: formation, DENSE INTERSTELLAR CLOUDS, Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], astrochemistry, Molecular cloud, Photodissociation, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, MOLECULAR-IONS, molecular processes, L1544, 13. Climate action, Space and Planetary Science, radiative transfer, Astrophysics of Galaxies (astro-ph.GA), ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, PRE-STELLAR CORES, ABUNDANCE, line: formation, DEPLETION, Water vapor, Galaxy Astrophysics
Abstract

SWAS and Odin provided stringent upper limits on the gas phase water abundance of dark clouds (x(H2O) < 7x10^-9). We investigate the chemistry of water vapor in starless cores beyond the previous upper limits using the highly improved angular resolution and sensitivity of Herschel and measure the abundance of water vapor during evolutionary stages just preceding star formation. High spectral resolution observations of the fundamental ortho water (o-H2O) transition (557 GHz) were carried out with Herschel HIFI toward two starless cores: B68, a Bok globule, and L1544, a prestellar core embedded in the Taurus molecular cloud complex. The rms in the brightness temperature measured for the B68 and L1544 spectra is 2.0 and 2.2 mK, respectively, in a velocity bin of 0.59 km s^-1. The continuum level is 3.5+/-0.2 mK in B68 and 11.4+/-0.4 mK in L1544. No significant feature is detected in B68 and the 3 sigma upper limit is consistent with a column density of o-H2O N(o-H2O) < 2.5x10^13 cm^-2, or a fractional abundance x(o-H2O) < 1.3x10^-9, more than an order of magnitude lower than the SWAS upper limit on this source. The L1544 spectrum shows an absorption feature at a 5 sigma level from which we obtain the first value of the o-H2O column density ever measured in dark clouds: N(o-H2O) = (8+/-4)x10^12 cm^-2. The corresponding fractional abundance is x(o-H2O) ~ 5x10^-9 at radii > 7000 AU and ~2x10^-10 toward the center. The radiative transfer analysis shows that this is consistent with a x(o-H2O) profile peaking at ~10^-8, 0.1 pc away from the core center, where both freeze-out and photodissociation are negligible. Herschel has provided the first measurement of water vapor in dark regions. Prestellar cores such as L1544 (with their high central densities, strong continuum, and large envelopes) are very promising tools to finally shed light on the solid/vapor balance of water in molecular clouds., Accepted for publication in Astronomy and Astrophysics (HIFI first results issue)

Published
2010

22. Screening uptake of colonoscopy versus fecal immunochemical testing in first-degree relatives of patients with non-syndromic colorectal cancer: A multicenter, open-label, parallel-group, randomized trial (ParCoFit study).

Author

González-López N, Quintero E, Gimeno-Garcia AZ, Bujanda L, Banales J, Cubiella J, Salve-Bouzo M, Herrero-Rivas JM, Cid-Delgado E, Alvarez-Sanchez V, Ledo-Rodríguez A, de-Castro-Parga ML, Fernández-Poceiro R, Sanromán-Álvarez L, Santiago-Garcia J, Herreros-de-Tejada A, Ocaña-Bombardo T, Balaguer F, Rodríguez-Soler M, Jover R, Ponce M, Alvarez-Urturi C, Bessa X, Roncales MP, Sopeña F, Lanas A, Nicolás-Pérez D, Adrián-de-Ganzo Z, Carrillo-Palau M, and González-Dávila E

Subjects
Humans, Colonoscopy methods, Risk Factors, Siblings, Mass Screening methods, Early Detection of Cancer methods, Colorectal Neoplasms epidemiology
Abstract

Background: Colonoscopy screening is underused by first-degree relatives (FDRs) of patients with non-syndromic colorectal cancer (CRC) with screening completion rates below 50%. Studies conducted in FDR referred for screening suggest that fecal immunochemical testing (FIT) was not inferior to colonoscopy in terms of diagnostic yield and tumor staging, but screening uptake of FIT has not yet been tested in this population. In this study, we investigated whether the uptake of FIT screening is superior to the uptake of colonoscopy screening in the familial-risk population, with an equivalent effect on CRC detection., Methods and Findings: This open-label, parallel-group, randomized trial was conducted in 12 Spanish centers between February 2016 and December 2021. Eligible individuals included asymptomatic FDR of index cases <60 years, siblings or ≥2 FDR with CRC. The primary outcome was to compare screening uptake between colonoscopy and FIT. The secondary outcome was to determine the efficacy of each strategy to detect advanced colorectal neoplasia (adenoma or serrated polyps ≥10 mm, polyps with tubulovillous architecture, high-grade dysplasia, and/or CRC). Screening-naïve FDR were randomized (1:1) to one-time colonoscopy versus annual FIT during 3 consecutive years followed by a work-up colonoscopy in the case of a positive test. Randomization was performed before signing the informed consent using computer-generated allocation algorithm based on stratified block randomization. Multivariable regression analysis was performed by intention-to-screen. On December 31, 2019, when 81% of the estimated sample size was reached, the trial was terminated prematurely after an interim analysis for futility. Study outcomes were further analyzed through 2-year follow-up. The main limitation of this study was the impossibility of collecting information on eligible individuals who declined to participate. A total of 1,790 FDR of 460 index cases were evaluated for inclusion, of whom 870 were assigned to undergo one-time colonoscopy (n = 431) or FIT (n = 439). Of them, 383 (44.0%) attended the appointment and signed the informed consent: 147/431 (34.1%) FDR received colonoscopy-based screening and 158/439 (35.9%) underwent FIT-based screening (odds ratio [OR] 1.08; 95% confidence intervals [CI] [0.82, 1.44], p = 0.564). The detection rate of advanced colorectal neoplasia was significantly higher in the colonoscopy group than in the FIT group (OR 3.64, 95% CI [1.55, 8.53], p = 0.003). Study outcomes did not change throughout follow-up., Conclusions: In this study, compared to colonoscopy, FIT screening did not improve screening uptake by individuals at high risk of CRC, resulting in less detection of advanced colorectal neoplasia. Further studies are needed to assess how screening uptake could be improved in this high-risk group, including by inclusion in population-based screening programs., Trial Registration: This trial was registered with ClinicalTrials.gov (NCT02567045)., Competing Interests: EQ and AL received an honorarium for consultancy from Sysmex (2017–2020). FB received endoscopic equipment on loan of Fujifilm, received an honorarium for consultancy from Sysmex (2017–2020) and editorial fee from Elsevier as editor of Gastroenterologia y Hepatologia. The other authors declare no conflict of interest regarding this study., (Copyright: © 2023 González-López et al. This is an open access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited.)

Published
2023
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23. Modulation of DRG neurons response to semaphorin 3A via substrate stiffness.

Author

Vela-Alcantara AM, Rios-Ramirez A, Santiago-Garcia J, Rodriguez-Alba JC, and Tamariz Domínguez E

Subjects
Nerve Tissue Proteins genetics, Neurons metabolism, Neuropilin-1 genetics, Tubulin metabolism, Ganglia, Spinal metabolism, Semaphorin-3A metabolism
Abstract

Semaphorin 3A (Sema3a) is a chemotropic protein that acts as a neuronal guidance cue and plays a major role in dorsal root ganglion (DRG) sensory neurons projection during embryo development. The present study evaluated the impact of stiffness in the repulsive response of DRG neurons to Sema3a when cultured over substrates of variable stiffness. Stiffness modified DRG neurons morphology and regulated their response to Sema3a, reducing the collapse of growth cones when they were cultured on softer substrates. Sema3a receptors expression was also regulated by stiffness, neuropilin-1 was overexpressed and plexin A4 mRNA was downregulated in stiffer substrates. Cytoskeleton distribution was also modified by stiffness. In softer substrates, βIII-tubulin and actin co-localized up to the leading edge of the growth cones, and as the substrate became stiffer, βIII-tubulin was confined to the transition and peripheral domains of the growth cone. Moreover, a decrease in the α-actinin adaptor protein was also observed in softer substrates. Our results show that substrate stiffness plays an important role in regulating the collapse response to Sema3a and that the modulation of cytoskeleton distribution and Sema3a receptors expression are related to the differential collapse responses of the growth cones., Competing Interests: Declaration of competing interest The authors declare that there are no competing interests associated with the manuscript., (Copyright © 2022 Elsevier B.V. All rights reserved.)

Published
2022
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25. Aneuploidy in targeted endoscopic biopsies outperforms other tissue biomarkers in the prediction of histologic progression of Barrett's oesophagus: A multi-centre prospective cohort study.

Author

Hadjinicolaou AV, van Munster SN, Achilleos A, Santiago Garcia J, Killcoyne S, Ragunath K, Bergman JJGHM, Fitzgerald RC, and di Pietro M

Subjects
Aged, Aged, 80 and over, Barrett Esophagus genetics, Core Binding Factor Alpha 3 Subunit genetics, Cyclin A genetics, Cyclin-Dependent Kinase Inhibitor p16 genetics, Disease Progression, Endoscopy, Female, Humans, Logistic Models, Male, Membrane Proteins genetics, Middle Aged, Neoplasm Proteins genetics, Prospective Studies, Tumor Suppressor Protein p53 genetics, Adenocarcinoma genetics, Aneuploidy, Barrett Esophagus pathology, Esophageal Neoplasms genetics, Genetic Markers
Abstract

Background: The cancer risk in Barrett's oesophagus (BO) is difficult to estimate. Histologic dysplasia has strong predictive power, but can be missed by random biopsies. Other clinical parameters have limited utility for risk stratification. We aimed to assess whether a molecular biomarker panel on targeted biopsies can predict neoplastic progression of BO., Methods: 203 patients with BO were tested at index endoscopy for 9 biomarkers (p53 and cyclin A expression; aneuploidy and tetraploidy; CDKN2A (p16), RUNX3 and HPP1 hypermethylation; 9p and 17p loss of heterozygosity) on autofluorescence-targeted biopsies and followed-up prospectively. Data comparing progressors to non-progressors were evaluated by univariate and multivariate analyses using survival curves, Cox-proportional hazards and logistic regression models., Findings: 127 patients without high-grade dysplasia (HGD) or oesophageal adenocarcinoma (OAC) at index endoscopy were included, of which 42 had evidence of any histologic progression over time. Aneuploidy was the only predictor of progression from non-dysplastic BO (NDBO) to any grade of neoplasia (p = 0.013) and HGD/OAC (p = 0.002). Aberrant p53 expression correlated with risk of short-term progression within 12 months, with an odds ratio of 6.0 (95% CI: 3.1-11.2). A panel comprising aneuploidy and p53 had an area under the receiving operator characteristics curve of 0.68 (95% CI: 0.59-0.77) for prediction of any progression., Interpretation: Aneuploidy is the only biomarker that predicts neoplastic progression of NDBO. Aberrant p53 expression suggests prevalent dysplasia, which might have been missed by random biopsies, and warrants early follow up., Competing Interests: Declaration of Competing Interest KR reports grants, personal fees and non-financial support from Olympus, outside the submitted work. JB reports grants from Olympus Endoscopy, outside the submitted work. Other authors have nothing to disclose., (Copyright © 2020 The Author(s). Published by Elsevier B.V. All rights reserved.)

Published
2020
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26. A dinucleotide deletion in amyloid precursor protein (APP) mRNA associated with sporadic Alzheimer's disease results in efficient secretion of truncated APP isoforms from neuroblastoma cell cultures.

Author

Hersberger M, Santiago-Garcia J, Patarroyo-White S, Yan J, and Xu X

Subjects
Amyloid beta-Protein Precursor biosynthesis, Animals, DNA, Complementary, Green Fluorescent Proteins, Humans, Luminescent Proteins analysis, Luminescent Proteins genetics, Molecular Weight, Neuroblastoma, Protein Isoforms biosynthesis, Protein Isoforms genetics, Rats, Recombinant Fusion Proteins biosynthesis, Subcellular Fractions metabolism, Subcellular Fractions ultrastructure, Transfection, Tumor Cells, Cultured, Alzheimer Disease genetics, Amyloid beta-Protein Precursor genetics, RNA, Messenger genetics, Sequence Deletion
Abstract

Recently, two dinucleotide deletions were detected in the mRNA of the amyloid precursor protein (APP) from cerebral cortex neurons of patients with sporadic Alzheimer's disease (AD) or Down's syndrome. These deletions resulted in truncation of APP, producing an APP isoform with a 38-kDa N-terminus and a novel carboxyl terminus (APP+1). We investigated the subcellular localization and the processing of APP+1 in the neuroblastoma cell line B103. cDNA constructs were generated encoding fusion proteins of APP+1 or full-length APP with the enhanced green fluorescent protein (eGFP). In transient transfection experiments using B103 cells, the APP+1-eGFP fusion protein showed a reticular localization with intense staining in the Golgi complex. Unlike full-length APP fused to eGFP, the APP+1-eGFP fusion protein did not localize to the perinuclear area or to the plasma membrane. Western blot analysis of cell extracts confirmed the translation of the expected fusion proteins. Analysis of the supernatant by western blot indicated that the APP+1-eGFP fusion protein was efficiently secreted from B103 cells, whereas the secreted form of full-length APP fusion protein (APPs) was hardly detectable. Thus, both dinucleotide deletions in the APP mRNA result in truncated APP+1 that is not membrane associated and is readily secreted from neurons.

Published
2001
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