Christiane Armand

Propos autour de l'exposition « Houston we've had a problem ! » à la Galerie Karima Celestin (du 29 mai au 12 juillet 2014. Commissariat : Karima Célestin)

The purpose of this thesis is to investigate the relation between sound and image in the actual artistic works and especially from video art and to try to determine how this linkage provides violence, emotion, fascination but also how it comes within the scope of the contest of the thinking emergence, the meaning shifting, the work reception by the...

A high signal-to-noise 52-90 mu m spectrum is presented for the central part of the Sagittarius B2 complex. The data were obtained with the Long Wavelength Spectrometer on board the Infrared Space Observatory (ISO). The [O I] 63 mu m line is detected in absorption even at the grating spectral resolution of 0.29 mu m. A lower limit for the column de...

We present an ISO Long Wavelength Spectrometer (LWS) grating spectrum of the carbon-rich circumstellar envelope -CSE- of IRC+10216 between 43 and 197 μm. The spectrum consists of strong dust emission plus a forest of emission lines from CO, HCN, H13CN and vibrationally excited HCN (ν2=11,20,2 and ν1,3=1). All the CO lines between J=14-13 and J=39-3...

The first detection of thermal water emission from a Herbig-Haro object is presented. The observations were performed with the Lws (Long Wavelength Spectrograph) aboard ISO (Infrared Space Observatory). Besides H2O, rotational lines of CO are present in the spectrum of HH 54. These high-J CO lines are used to derive the physical model parameters of...

The spectrum of Saturn from 43 to 197μm was measured with the ISO Long Wavelength Spectrometer (LWS) during the performance verification phase of the mission. The measurements were made using the LWS in grating mode, with spectral resolutions of 0.29μm from 43 to 90μm and 0.6μm from 90 to 197μm. The spectrum was compared with an atmospheric radiati...

The R(1) rotational line of HD at 56.23μm has been detected for the first time on Saturn using the Long Wavelength Spectrometer (LWS) on board the Infrared Space Observatory (ISO). The measurements were made using the LWS in Fabry-Perot mode in January 1996 during the ISO performance verification phase. The measured spectrum has been compared with...

We present the first far infrared spectra of the Herbig Haro objects HH 52-53-54 and of IRAS 12496-7650, all located in the nearby star forming region known as Chamaleon II dark cloud, obtained with the Long Wavelength Spectrometer (LWS) onboard the Infrared Space Observatory (ISO). The richest spectrum is found in HH 54, showing molecular transiti...

Grating spectra, covering the wavelength range 45 to 187μm have been taken with the ISO Long Wavelength Spectrometer (LWS) at a series of pointing positions over the S 140 region, centred on the cluster of embedded young stellar objects at the south-west corner of the L1204 molecular cloud. Extended emission from [CII]158μm and [OI]63μm is seen, pe...

The wavelength and flux calibration, and the in-orbit performance of the Infrared Space Observatory Long-Wavelength Spectrometer (LWS) are described. The LWS calibration is mostly complete and the instrument's performance in orbit is largely as expected before launch. The effects of ionising radiation on the detectors, and the techniques used to mi...

We present the first far infrared spectra of the Herbig Haro objects HH 52-53-54 and of IRAS 12496-7650, all located in the nearby star forming region known as Chamaleon II dark cloud, obtained with the Long Wavelength Spectrometer (LWS) onboard the Infrared Space Observatory (ISO). The richest spectrum is found in HH 54, showing molecular transiti...

We present the first far-infrared spectrum of the IRAS source associated with IC 1396N, located in the HII region IC 1396 together with submillimeter and millimeter photometry. A rich spectrum of CO, OH, and H_2_O lines are detected in the ISO-LWS spectrum, indicative of a warm, dense region, probably shock excited, around the source. Among the fin...

We present an ISO Long Wavelength Spectrometer (LWS) grating spectrum of the carbon-rich proto-planetary nebula AFGL 2688 between 43 and 194mum. The far-infrared spectrum of AFGL 2688 is dominated by strong rotational transitions of CO which are detected from J=14-13 up to J=23-22. The atomic fine structure lines [O I] and [C II] are not detected....

We present an ISO Long Wavelength Spectrometer (LWS) grating spectrum of the oxygen-rich AGB star W Hya from 43-197mum. The spectrum is dominated by a forest of water vapour emission lines, confirming that H_2_O molecules are the dominant coolants of the winds of these stars. We have constructed an outflow model for the H_2_O spectrum of W Hya, whi...

The Long-Wavelength Spectrometer (LWS) is one of two complementary spectrometers aboard the European Space Agency's Infrared Space Observatory (ISO) (Kessler et al., 1996). It operates over the wavelength range 43 - 196.9 ensuremath ensuremathmuensuremath<?iensuremath>m at either medium (about 150 to 200) or high (6800 to 9700) spectral resolving p...

We present a high signal-to-noise ISO Long Wavelength Spectrometer (LWS) grating spectrum of the planetary nebula NGC 7027 from 43-194mum. In total 40 emission lines have been detected, with 30 identified. From the ionized region, we observe fine-structure lines from [N II], [N III] and [O III]. The [O I] and [C II] fine-structure lines from the ph...

Grating spectra, covering the wavelength range 45 to 187μm have been taken with the ISO Long Wavelength Spectrometer (LWS) at a series of pointing positions over the S 140 region, centred on the cluster of embedded young stellar objects at the south-west corner of the L1204 molecular cloud. Extended emission from [CII]158μm and [OI]63μm is seen, pe...

Infrared Space Observatory (ISO) Long Wavelength Spectrometer (LWS) and ground-based Fabry-Perot imaging spectroscopic observations are used to penetrate the extinction to the powerful burst of star formation that has occurred in the extranuclear molecular cloud complex in the galaxy overlap region of the galaxies NGC 4038/39 ("The Antennae"). Para...

We present near-infrared spectrophotometry of five southern ultracompact (UC) HII regions, namely: IRAS 08546-4254, IRAS 12073-6233, IRAS 15408-5356, IRAS 17200-3550 and IRAS 17455-2800. The spectra which cover parts of the range 1.25 to 4.1 μm display the emission lines of atomic and molecular hydrogen, those of He I, He II and [Fe II]. Near-infra...

We have used galaxy counts obtained at 2000 A down to a magnitude of 18.5 to calculate the ultraviolet integrated light of galaxies. The calculation is based on models developed to interpret the galaxy counts. Because of various sources of uncertainty, the extrapolated values lie in the range 40 - 130 photons/sq cm/s/A/sr. This extrapolated intensi...

A prediction of galaxy counts at 2000 A and m2000 - B color distributions is elaborated from published spectral energy distributions and evolution models of galaxies. The comparison of the predictions to the observations at 2000 A is used to derive constraints on the local density of star-forming galaxies and their recent evolution. The data indica...

Le travail présenté ici concerne la dérivation et l'analyse de comptages de galaxies dans l'ultraviolet lointain (UV) (2000 A) dans l'intervalle de magnitudes UV 15-18.5, à partir d'observations obtenues avec l'expérience Foca embarquée en ballon. Une prédiction des comptages de galaxies à 2000 A et des distributions en couleur m2000-B est élaborée...

We present UBV photometry of the stellar cluster associated with N59A, a dusty H II region in the LMC. N59A's main detected source of ionization is an O5V (or possibly earlier type) star with a visual extinction of 1.2 mag. N59A also contains fifteen O-B3 stars that may contribute to the ionization; these stars are affected by greatly differing amo...

Four high galactic latitude fields imaged at 2000 A with a 40-cm balloon-borne telescope have been used to perform galaxy counts in the range of UV magnitudes 15.0-18.5. The UV galaxy counts are higher than those measured in the U Johnson band and similar to those in the B, at the same F(lambda). The detected galaxies present negative m(2000)-b col...

Individual galaxy counts at 2000 A derived from ultraviolet (UV) images obtained with a 40-cm balloon-borne telescope are presented and discussed. The galaxy number counts are high, with a steep differential log-counts slope. The detected galaxies show very blue m2000-b colours, typical of late type spirals. Galaxies brighter than m2000 = 18.5 cont...