References of "Hutsemekers, Damien"
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See detailOptical Spectroscopy of the B and C Fragments of Comet 73P/Schwassmann-Wachmann 3 at the ESO VLT
Jehin, Emmanuel ULg; Manfroid, Jean ULg; Kawakita, H. et al

in LPI contribution 1405 (2008)

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See detailA Multi-Wavelength Simultaneous Study of the Composition of the Halley-Family Comet 8P/Tuttle at the VLT
Bockelée-Morvan, Dominique; Dello Russo, N.; Jehin, Emmanuel ULg et al

in LPI contribution 1405 (2008)

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See detailA Fluorescence Model for 12C13C in Comets
Rousselot, P.; Jehin, Emmanuel ULg; Manfroid, Jean ULg et al

in LPI contribution 1405 (2008)

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See detailCarbon and Nitrogen Isotopic Ratios in Comets
Jehin, Emmanuel ULg; Manfroid, Jean ULg; Hutsemekers, Damien ULg et al

in LPI contribution 1405 (2008)

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See detailUnderstanding the relations between QSOs and their host galaxies from combined HST imaging and VLT spectroscopy
Letawe, Yannick ULg; Magain, Pierre ULg; Letawe, Géraldine ULg et al

in Astrophysical Journal (2008), 679(2), 967-983

The host galaxies of six nearby QSOs are studied on the basis of high-resolution HST optical images and spatially resolved VLT slit spectra. The gas ionization and velocity are mapped as a function of the ... [more ▼]

The host galaxies of six nearby QSOs are studied on the basis of high-resolution HST optical images and spatially resolved VLT slit spectra. The gas ionization and velocity are mapped as a function of the distance to the central QSO. In the majority of the cases, the QSO significantly contributes to the gas ionization in its whole host galaxy, and sometimes even outside. Reflection or scattering of the QSO H alpha line from remote regions of the galaxy is detected in several instances. The line shifts show that, in all cases, the matter responsible for the light reflection moves away from the QSO, likely accelerated by its radiation pressure. The two faintest QSOs reside in spirals, with some signs of a past gravitational perturbation. One of the intermediate-luminosity QSOs resides in a massive elliptical containing gas ionized (and probably pushed away) by the QSO radiation. The other medium-power object is found in a spiral galaxy displaying complex velocity structure, with the central QSO moving with respect to the bulge, probably as a result of a galactic collision. The two most powerful objects are involved in violent gravitational interactions, and one of them has no detected host. These results suggest that (1) large-scale phenomena, such as galactic collisions, are closely related to the triggering and the feeding of the QSO and (2) once ignited, the QSO has significant influence on its large-scale neighborhood ( often the whole host and sometimes further away). [less ▲]

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See detailQSO Type1/Type2 dichotomy (Borguet+, 2008)
Borguet, Benoît ULg; Hutsemekers, Damien ULg; Letawe, Géraldine ULg et al

Textual, factual or bibliographical database (2007)

This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of ... [more ▼]

This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references. (2 data files). [less ▲]

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See detailCircular Polarimetry Now Offered at EFOSC2
Saviane, Ivo; Piirola, Vilppu; Bagnulo, Stefano et al

in The Messenger (2007), 129

Starting from period P79, circular polarimetry measurements can be carried out with EFOSC2 at the ESO 3.6-m telescope. Here we describe the motivations behind the upgrade of the instrument, and a few ... [more ▼]

Starting from period P79, circular polarimetry measurements can be carried out with EFOSC2 at the ESO 3.6-m telescope. Here we describe the motivations behind the upgrade of the instrument, and a few results from the commissioning runs are used to show the excellent performance of the new polarimetry unit. [less ▲]

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See detailAcceleration and Substructure Constraints in a Quasar Outflow
Hall, Patrick B; Sadavoy, Sarah I; Hutsemekers, Damien ULg et al

in Astrophysical Journal (2007), 665

We present observations of probable line-of-sight acceleration of a broad absorption trough of C IV in the quasar SDSS J024221.87+004912.6. We also discuss how the velocity overlap of two other outflowing ... [more ▼]

We present observations of probable line-of-sight acceleration of a broad absorption trough of C IV in the quasar SDSS J024221.87+004912.6. We also discuss how the velocity overlap of two other outflowing systems in the same object constrains the properties of the outflows. The Si IV doublet in each system has one unblended transition and one transition that overlaps with absorption from the other system. The residual flux in the overlapping trough is well fit by the product of the residual fluxes in the unblended troughs. For these optically thick systems to yield such a result, at least one of them must consist of individual subunits, rather than being a single structure with velocity-dependent coverage of the source. If these subunits are identical, opaque, spherical clouds, we estimate the cloud radius to be r~=3.9×10[SUP]15[/SUP] cm. If they are identical, opaque, linear filaments, we estimate their width to be w~=6.5×10[SUP]14[/SUP] cm. These subunits are observed to cover the Mg II broad emission-line region of the quasar, at which distance from the black hole the above filament width is equal to the predicted scale height of the outer atmosphere of a thin accretion disk. Insofar as that scale height is a natural size scale for structures originating in an accretion disk, these observations are evidence that the accretion disk can be a source of quasar absorption systems. This paper is based on data from ESO program 075.B-0190(A). [less ▲]

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See detailMulti-wavelength study of the gravitational lens system RXS J1131-1231 - III. Long slit spectroscopy: micro-lensing probes the QSO structure
Sluse, Dominique ULg; Claeskens, Jean-François ULg; Hutsemekers, Damien ULg et al

in Astronomy and Astrophysics (2007), 468(3), 885-901

Aims. We discuss and characterize micro-lensing among the 3 brightest lensed images (A-B-C) of the gravitational lens system RXS J1131-1231 (a quadruply imaged AGN) by means of long slit optical and NIR ... [more ▼]

Aims. We discuss and characterize micro-lensing among the 3 brightest lensed images (A-B-C) of the gravitational lens system RXS J1131-1231 (a quadruply imaged AGN) by means of long slit optical and NIR spectroscopy. Qualitative constraints on the size of different emission regions are derived. We also perform a spectroscopic study of two field galaxies located within 1.6 arcmin radius from the lens. Methods. We decompose the spectra into their individual emission components using a multi-component fitting approach. A complementary decomposition of the spectra enables us to isolate the macro-lensed fraction of the spectra independently of any spectral modelling. Results. 1. The data support micro-lensing de-amplification of images A and C. Not only is the continuum emission microlensed in those images but also a fraction of the Broad Line emitting Region (BLR). 2. Micro-lensing of a very broad component of Mg II emission line suggests that the corresponding emission occurs in a region more compact than the other components of the emission line. 3. We find evidence that a large fraction of the Fe II emission arises in the outer parts of the BLR. We also find a very compact emitting region in the ranges 3080-3540 angstrom and 4630-4800 angstrom that is likely associated with Fe II. 4. The [O III] narrow emission line regions are partly spatially resolved. This enables us to put a lower limit of similar to 110h(-1) pc on their intrinsic size. 5. Analysis of Mg II absorption found in the spectra indicates that the absorbing medium is intrinsic to the quasar, has a covering factor of 20%, and is constituted of small clouds homogeneously distributed in front of the continuum and BLRs. 6. Two neighbour galaxies are detected at redshifts z = 0.10 and z = 0.289. These galaxies are possible members of galaxy groups reported at those redshifts. [less ▲]

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See detailNuclear spin temperature of ammonia in Comet 9P/Tempel 1 before and after the Deep Impact event
Kawakita, Hideyo; Jehin, Emmanuel ULg; Manfroid, Jean ULg et al

in Icarus (2007), 187

The Deep Impact mission succeeded in excavating inner materials from the nucleus of Comet 9P/Tempel 1 on 2005 July 04 (at 05:52 UT). Comet 9P/Tempel 1 is one of Jupiter family short period comets, which ... [more ▼]

The Deep Impact mission succeeded in excavating inner materials from the nucleus of Comet 9P/Tempel 1 on 2005 July 04 (at 05:52 UT). Comet 9P/Tempel 1 is one of Jupiter family short period comets, which might originate in the Kuiper belt region in the solar nebula. In order to characterize the comet and to support the mission from the ground-based observatory, optical high-dispersion spectroscopic observations were carried out with the echelle spectrograph (UVES) mounted on the 8-m telescope VLT (UT2) before and after the Deep Impact event. Ortho-to-para abundance ratios (OPRs) of cometary ammonia were determined from the NH[SUB]2[/SUB] emission spectra. The OPRs of ammonia on July 3.996 UT and 4.997 UT were derived to be 1.28±0.07 (nuclear spin temperature: T[SUB][/SUB]=24±2 K) and 1.26±0.08 (T[SUB][/SUB]=25±2 K), respectively. There is no significant change between before and after the impact. Actually, most materials ejected from the impact site could have moved away from the nucleus on July 4.997 UT, about 17 h after the impact. However, a small fraction of the ejected materials might remain in the slit of UVES instrument at that time because an excess of about 20% in the NH[SUB]2[/SUB] emission flux is observed above the normal activity level was found [Manfroid, J., Hutsemékers, D., Jehin, E., Cochran, A.L., Arpigny, C., Jackson, W.M., Meech, K.J., Schulz, R., Zucconi, J.-M., 2007. Icarus. This issue]. If the excess of NH[SUB]2[/SUB] on July 04.997 UT was produced from icy materials excavated by the Deep Impact, then an upper-limit of the ammonia OPR would be 1.75 (T[SUB][/SUB]>17 K) for those materials. On the other hand, the OPR of ammonia produced from the quiescent sources was similar to that of the Oort cloud comets observed so far. This fact may imply that physical conditions where cometary ices formed were similar between Comet 9P/Tempel 1 and the Oort cloud comets. [less ▲]

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See detailThe impact and rotational light curves of Comet 9P/Tempel 1
Manfroid, Jean ULg; Hutsemekers, Damien ULg; Jehin, Emmanuel ULg et al

in Icarus: International Journal of Solar System Studies (2007), 187

UVES and HIRES high-resolution spectra of Comet 9P/Tempel 1 are used to investigate the impact and rotational light curves of various species with a view toward building a simple model of the distribution ... [more ▼]

UVES and HIRES high-resolution spectra of Comet 9P/Tempel 1 are used to investigate the impact and rotational light curves of various species with a view toward building a simple model of the distribution and activity of the sources. The emission by OH, NH, CN, C[SUB]3[/SUB], CH, C[SUB]2[/SUB], NH[SUB]2[/SUB], and OI, are analyzed, as well as the light scattered by the dust. It is found that a simple model reproduces fairly well the impact light curves of all species combining the production of the observed molecules and the expansion of the material throughout the slit. The impact light curves are consistent with velocities of 400 600 m/s. Their modeling requires a three-step dissociation sequence ``Grand-Parent --> Parent --> Daughter'' to produce the observed molecules. The rotational light curve for each species is explained in terms of a single model with three sources. The dust component can however not easily be explained that way. [less ▲]

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See detailComet C/2006 P1 (McNaught)
Jehin, Emmanuel ULg; Manfroid, Jean ULg; Snodgrass, C. et al

in Central Bureau Electronic Telegrams (CBETs) (2007), 832

CBET 832 available at Central Bureau for Astronomical Telegrams.

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See detailThe impact and rotational light curves of Comet 9P/Tempel 1
Manfroid, Jean ULg; Hutsemekers, Damien ULg; Jehin, Emmanuel ULg et al

in Icarus: International Journal of Solar System Studies (2007), 191

UVES and HIRES high-resolution spectra of Comet 9P/Tempel 1 are used to investigate the impact and rotational light curves of various species with a view toward building a simple model of the distribution ... [more ▼]

UVES and HIRES high-resolution spectra of Comet 9P/Tempel 1 are used to investigate the impact and rotational light curves of various species with a view toward building a simple model of the distribution and activity of the sources. The emission by OH, NH, CN, C[SUB]3[/SUB], CH, C[SUB]2[/SUB], NH[SUB]2[/SUB], and OI, are analyzed, as well as the light scattered by the dust. It is found that a simple model reproduces fairly well the impact light curves of all species combining the production of the observed molecules and the expansion of the material throughout the slit. The impact light curves are consistent with velocities of 400 600 m/s. Their modeling requires a three-step dissociation sequence ``Grand-Parent --> Parent --> Daughter'' to produce the observed molecules. The rotational light curve for each species is explained in terms of a single model with three sources. The dust component can however not easily be explained that way. [less ▲]

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See detailComet C/2006 P1 (McNaught)
Snodgrass, C.; Fitzsimmons, A.; Hainaut, O. et al

in Central Bureau Electronic Telegrams (CBETs) (2007), 832

CBET 832 available at Central Bureau for Astronomical Telegrams.

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See detailNuclear spin temperature of ammonia in Comet 9P/Tempel 1 before and after the Deep Impact event
Kawakita, Hideyo; Jehin, Emmanuel ULg; Manfroid, Jean ULg et al

in Icarus: International Journal of Solar System Studies (2007), 191

The Deep Impact mission succeeded in excavating inner materials from the nucleus of Comet 9P/Tempel 1 on 2005 July 04 (at 05:52 UT). Comet 9P/Tempel 1 is one of Jupiter family short period comets, which ... [more ▼]

The Deep Impact mission succeeded in excavating inner materials from the nucleus of Comet 9P/Tempel 1 on 2005 July 04 (at 05:52 UT). Comet 9P/Tempel 1 is one of Jupiter family short period comets, which might originate in the Kuiper belt region in the solar nebula. In order to characterize the comet and to support the mission from the ground-based observatory, optical high-dispersion spectroscopic observations were carried out with the echelle spectrograph (UVES) mounted on the 8-m telescope VLT (UT2) before and after the Deep Impact event. Ortho-to-para abundance ratios (OPRs) of cometary ammonia were determined from the NH[SUB]2[/SUB] emission spectra. The OPRs of ammonia on July 3.996 UT and 4.997 UT were derived to be 1.28±0.07 (nuclear spin temperature: T[SUB][/SUB]=24±2 K) and 1.26±0.08 (T[SUB][/SUB]=25±2 K), respectively. There is no significant change between before and after the impact. Actually, most materials ejected from the impact site could have moved away from the nucleus on July 4.997 UT, about 17 h after the impact. However, a small fraction of the ejected materials might remain in the slit of UVES instrument at that time because an excess of about 20% in the NH[SUB]2[/SUB] emission flux is observed above the normal activity level was found [Manfroid, J., Hutsemékers, D., Jehin, E., Cochran, A.L., Arpigny, C., Jackson, W.M., Meech, K.J., Schulz, R., Zucconi, J.-M., 2007. Icarus. This issue]. If the excess of NH[SUB]2[/SUB] on July 04.997 UT was produced from icy materials excavated by the Deep Impact, then an upper-limit of the ammonia OPR would be 1.75 (T[SUB][/SUB]>17 K) for those materials. On the other hand, the OPR of ammonia produced from the quiescent sources was similar to that of the Oort cloud comets observed so far. This fact may imply that physical conditions where cometary ices formed were similar between Comet 9P/Tempel 1 and the Oort cloud comets. [less ▲]

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See detailThe Dusty Young Universe: photometry and spectroscopy of quasars at z > 2
Meisenheimer, K.; Hutsemekers, Damien ULg; Tacconi, L. et al

Poster (2007)

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See detailObservations of comet McNaught from La Silla
Snodgrass, C.; Jehin, Emmanuel ULg; Fitzsimmons, A. et al

Poster (2007)

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See detailThe Dusty Young Universe
Meisenheimer, K.; Dannerbauer, H.; Klaas, U. et al

Poster (2007)

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See detailThe atypical emission-line star Hen 3-209
Nazé, Yaël ULg; Rauw, Grégor ULg; Hutsemekers, Damien ULg et al

in Monthly Notices of the Royal Astronomical Society (2006), 371(4), 1594-1600

We analyse observations, spanning 15 yr, dedicated to the extreme emission-line object Hen 3-209. Our photometric data indicate that the luminosity of the star undergoes marked variations with a peak-to ... [more ▼]

We analyse observations, spanning 15 yr, dedicated to the extreme emission-line object Hen 3-209. Our photometric data indicate that the luminosity of the star undergoes marked variations with a peak-to-peak amplitude of 0.65 mag. These variations are recurrent, with a period of 16.093 +/- 0.005 d. The spectrum of Hen 3-209 is peculiar with many different lines (H I, He I, Fe II,. showing P Cygni profiles. The line profiles are apparently changing in harmony with the photometry. The spectrum also contains [O III] lines that display a saddle profile topped by three peaks, with a maximum separation of about 600 km s(-1). Hen 3-209 is most likely an evolved luminous object suffering from mass ejection events and maybe belonging to a binary system. [less ▲]

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