88,244 research outputs found
Fragmentation and disk formation in high-mass star formation: The IRAM large program CORE
No full textThe IRAM CORE large program combines data from NOEMA and the IRAM 30m telescope to study a diverse set of physical and chemical processes during the formation of high-mass stars. Here, we present a selected compilation of exciting results obtained during the survey
An experimental study on effects of fluoridated water on Abelmoschus esculentus var. Soh-198 (Lady Finger) Arshi Iram*
No full textAn experimental study of fluoride (F) accumulation in Abelmoschus esculentus var. Soh-198 and its effect on the growth and crop yield was conducted in a pot experiment. Eight different concentrations of F in the water were used for irrigation ranging from 2 to 14 ppm with distilled water as the control. Potentiometric determinations of the F content in different parts of the plant were made 45, 60, and 120 days after sowing the seeds (first, second, and third harvest, respectively). At the third harvest the highest mean plant part concentrations of F were recorded with 14 ppm F in the irrigation water: 9.0638 mg/kg in the roots, 5.6896 mg/kg in shoot, 4.5348 mg/kg in leaf and 3.563 mg/kg in fruit
The Néel IRAM KID Arrays (NIKA)
No full textWe are developing an instrument based on Kinetic Inductance Detectors (KID) known as the N,el IRAM KID Array (NIKA). Leveraging the experience gained from the first generation NIKA in 2009, an improved, dual-band (150 GHz and 240 GHz) instrument has been designed and tested at the Institut of RadioAstronomie Millimetrique (IRAM) 30-meter telescope in October 2010. The performances, in terms of sensitivity on-the-sky at 150 GHz, are already comparable to existing state-of-the-art bolometer-based instruments. NIKA represents thus the first real proof that KID are a viable technology for ground-based Astronomy. We will describe the instrument, the most recent results and the future plans for building a large resident mm-wave camera
IRAM spectra toward M33 Giant Molecular Clouds (Buchbender+, 2013)
No full textist.dat 7x180 List of sources and FITS files; sp/* 42. Individual FITS spectraVizieR On-line Data Catalog: J/A+A/549/A17. Originally published in: 2013A&A...549A..17BThe attached FITS spectra contain the reduced IRAM 30m spectra of the ground state transitions 12CO, 13CO, HCN and HCO+ towards 7 GMC in M33 that are presented in Figure 3 and Figure A.1 of the paper. The 12CO spectra of GMCs: GMC1, GMC26 and GMC91, that are archived here, were first presented in Rosolowsky et al. (2011MNRAS.415.1977R) and were observed with the A,B,C,D receiver of the IRAM 30m. All other spectra were observed with the EMIR receiver. The backends used were: the FTS spectrometer in case of 12CO and 13CO spectra and the WILMA autocorrelator in case of HCN and HCO+. All spectra have been resampled to the intrinsic resolution of the WILMA spectrometer, which is 2MHz. This frequency resolution corresponds to a velocity resolution of 5.4km/s for 12CO and 13CO and 6.7km/s for HCN and HCOp. In addition we provide the 12CO and 13CO spectra at higher resolution of 333kHz corresponding to ~1km/s velocity resolution. All spectra have a bandwidth of 300km/s each. The nomenclature of the files is: "ObjectName"-"Molecule"-"Resolution"[.fits] The observed sources and their designations are listed below. The FITS files are created by GILDAS/Class. (2 data files)
IRAM spectra toward M33 Giant Molecular Clouds (Buchbender+, 2013)
No full textist.dat 7x180 List of sources and FITS files; sp/* 42. Individual FITS spectraVizieR On-line Data Catalog: J/A+A/549/A17. Originally published in: 2013A&A...549A..17BThe attached FITS spectra contain the reduced IRAM 30m spectra of the ground state transitions 12CO, 13CO, HCN and HCO+ towards 7 GMC in M33 that are presented in Figure 3 and Figure A.1 of the paper. The 12CO spectra of GMCs: GMC1, GMC26 and GMC91, that are archived here, were first presented in Rosolowsky et al. (2011MNRAS.415.1977R) and were observed with the A,B,C,D receiver of the IRAM 30m. All other spectra were observed with the EMIR receiver. The backends used were: the FTS spectrometer in case of 12CO and 13CO spectra and the WILMA autocorrelator in case of HCN and HCO+. All spectra have been resampled to the intrinsic resolution of the WILMA spectrometer, which is 2MHz. This frequency resolution corresponds to a velocity resolution of 5.4km/s for 12CO and 13CO and 6.7km/s for HCN and HCOp. In addition we provide the 12CO and 13CO spectra at higher resolution of 333kHz corresponding to ~1km/s velocity resolution. All spectra have a bandwidth of 300km/s each. The nomenclature of the files is: "ObjectName"-"Molecule"-"Resolution"[.fits] The observed sources and their designations are listed below. The FITS files are created by GILDAS/Class. (2 data files)
IRAM spectra toward M33 Giant Molecular Clouds (Buchbender+, 2013)
No full textist.dat 7x180 List of sources and FITS files; sp/* 42. Individual FITS spectraVizieR On-line Data Catalog: J/A+A/549/A17. Originally published in: 2013A&A...549A..17BThe attached FITS spectra contain the reduced IRAM 30m spectra of the ground state transitions 12CO, 13CO, HCN and HCO+ towards 7 GMC in M33 that are presented in Figure 3 and Figure A.1 of the paper. The 12CO spectra of GMCs: GMC1, GMC26 and GMC91, that are archived here, were first presented in Rosolowsky et al. (2011MNRAS.415.1977R) and were observed with the A,B,C,D receiver of the IRAM 30m. All other spectra were observed with the EMIR receiver. The backends used were: the FTS spectrometer in case of 12CO and 13CO spectra and the WILMA autocorrelator in case of HCN and HCO+. All spectra have been resampled to the intrinsic resolution of the WILMA spectrometer, which is 2MHz. This frequency resolution corresponds to a velocity resolution of 5.4km/s for 12CO and 13CO and 6.7km/s for HCN and HCOp. In addition we provide the 12CO and 13CO spectra at higher resolution of 333kHz corresponding to ~1km/s velocity resolution. All spectra have a bandwidth of 300km/s each. The nomenclature of the files is: "ObjectName"-"Molecule"-"Resolution"[.fits] The observed sources and their designations are listed below. The FITS files are created by GILDAS/Class. (2 data files)
Variations on the Author
No full text“Variations on the Author” discusses two of Eduardo Coutinho’s recent films (Um Dia na Vida, from 2010, and Últimas Conversas, posthumously released in 2015) and their contribution to the general question of documentary authorship. The director’s filmography is characterized by a consistent yet self-effacing form of authorial self-inscription: Coutinho often features as an interviewer that rather than express opinions propels discourses; an interviewer that is good at listening. This mode of self-inscription characterizes him as an author who is not expressive but who is nonetheless markedly present on the screen. In Um Dia na Vida, however, Coutinho is completely absent form the image, while Últimas Conversas, on the contrary, includes a confessional prologue that moves the director from the margins to the center of his films. This article examines the ways in which these works stand out in the filmography of a director who offers new insights into the notion of cinematic authorship
Probing episodic accretion with chemistry: CALYPSO observations of the very-low-luminosity Class 0 protostar IRAM 04191+1522: Results from the CALYPSO IRAM-PdBI survey
No full textInternational audienceContext. The process of mass accretion in the earliest phases of star formation is still not fully understood: does the accretion rate smoothly decline with the age of the protostar or are there short, intermittent accretion bursts? The latter option would also yield the possibility for very low-luminosity objects (VeLLOs) to be precursors of solar-type stars, even though they do not seem to have sufficiently high accretion rates to reach stellar masses during their protostellar lifetime. Nevertheless, probing such intermittent events in the deeply embedded phase is not easy. Chemical signatures in the protostellar envelope can trace a past accretion burst.Aims. We aim to explore whether or not the observed C18O and N2H+ emission pattern towards the VeLLO IRAM 04191+1522 can be understood in the framework of a scenario where the emission is chemically tracing a past accretion burst.Methods. We used high-angular-resolution Plateau de Bure Interferometer (PdBI) observations of C18O and N2H+ towards IRAM 04191+1522 that were obtained as part of the CALYPSO IRAM Large Program (Continuum And Lines in Young ProtoStellar Objects). We model these observations using a chemical code with a time-dependent physical structure coupled with a radiative transfer module, where we allow for variations in the source luminosity.Results. We find that the N2H+ line emission shows a central hole, with the N2H+ emission peaking at a radius of about 10′′ (1400 au) from the source, while the C18O emission is compact (1.3′′ FWHM, corresponding to 182 au). The morphology of these two lines cannot be reproduced with a constant luminosity model based on the present-day internal luminosity (0.08 L⊙). However, the N2H+ peaks are consistent with a constant-luminosity model of 12 L⊙. Using a model with time-dependent temperature and density profiles, we show that the observed N2H+ peak emission could indeed be caused by a past accretion burst with a luminosity 150 times higher than the present-day luminosity. Such a burst should have occurred a couple of hundred years ago.Conclusions. We suggest that an accretion burst occurred in IRAM 04191+1522 in the recent past. If such bursts are common and sufficiently long in VeLLOs, they could lead to higher accretion onto the central object than their luminosity suggests. For IRAM 04191 in particular, our results yield an estimated final mass of 0.2–0.25 M⊙ by the end of the Class 0 phase, which would make this object a low-mass star rather than a brown dwarf. More generally, our analysis demonstrates that the combination of observations of N2H+ and C18O is a more reliable diagnostic of past outburst activity than C18O or N2H+ emission alone
NIKA 2: Next-generation continuum/polarized camera at the IRAM 30 m telescope and its prototype
No full textNIKA 2 (New Instrument of Kids Array) is a next generation continuum and polarized instrument successfully installed in October 2015 at the IRAM 30 m telescope on Pico-Veleta (Granada, Spain). NIKA 2 is a high resolution dual-band camera, operating with frequency multiplexed LEKIDs (Lumped Element Kinetic Inductance Detectors) cooled at 100 mK. Dual color images are obtained thanks to the simultaneous readout of a 1020 pixels array at 2 mm and 1140 x 2 pixels arrays at 1.15 mm with a final resolution of 18 and 12 arcsec respectively, and 6.5 arcmin of Field of View (FoV). The two arrays at 1.15 mm allow us to measure the linear polarization of the incoming light. This will place NIKA 2 as an instrument of choice to study the role of magnetic fields in the star formation process. The NIKA experiment, a prototype for NIKA 2 with a reduced number of detectors ( 400 LEKIDs) and FoV (1.8 arcmin), has been successfully operated at the IRAM 30 telescope in several open observational campaigns. The performance of the NIKA 2 polarization setup has been successfully validated with the NIKA prototype
The NIKA2 instrument at 30-m IRAM telescope: performance and results
No full textInternational audienceThe New IRAM KID Array 2 (NIKA 2) is a dual-band camera operating with three frequency multiplexed kilo-pixelsarrays of Lumped Element Kinetic Inductance Detectors (LEKID) cooled at 100 mK. NIKA is designed to observethe intensity and polarisation of the sky at 250 and 150 GHz from the IRAM 30 m telescope. It represents onestep further with respect the NIKA pathnder instrument which has already shown state-of-the-art detectors andphotometric performance. NIKA 2 is an IRAM resident instrument for studies of the Intra Cluster Medium fromintermediate to distant clusters and so for the follow-up of Planck satellite detected clusters, high redshift sourcesand quasars, early stages of star formation and nearby galaxies emission. We present an overview of the instrumentperformance and the rst scientic results
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