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In the caddisfly Molanna angustata, females produce a sex pheromone in glands with openings on the fifth sternite. Gas chromatographic analyses of pheromone gland extracts with electroantennographic detection revealed four major compounds that stimulated male antennae. These compounds were identified by means of gas chromatography-mass spectrometry and(More)
  • C Cáceres, V D Ivanov, D Minniti, D Naef, C Melo, E Mason +2 others
  • 2009
Currently the only technique sensitive to Earth mass planets around nearby stars (that are too close for microlensing) is the monitoring of the transit time variations of the transiting extrasolar planets. We search for additional planets in the systems of the hot Neptune GJ 436b, and the hot-Jupiter XO-1b, using high cadence observations in the J and K S(More)
This paper describes an approach to problem phrase extraction from texts that contain user experience with products. In contrast to other works, we propose a straightforward approach to problem phrase extraction based on syntactic and semantic connections between a problem indicator and mentions about the problem targets. In this paper, we discuss (i)(More)
  • J Borissova, C Bonatto, R Kurtev, J R A Clarke, F Peñaloza, S E Sale +24 others
  • 2011
Context. VISTA Variables in the Vía Láctea (VVV) is one of the six ESO Public Surveys operating on the new 4-meter Visible and Infrared Survey Telescope for Astronomy (VISTA). VVV is scanning the Milky Way bulge and an adjacent section of the disk, where star formation activity is high. One of the principal goals of the VVV Survey is to find new star(More)
  • R K Saito, M Hempel, D Minniti, P W Lucas, M Rejkuba, I Toledo +40 others
  • 2011
Context. The ESO Public Survey VISTA Variables in the Vía Láctea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for ∼ 5 years. Aims. In this paper we describe the progress of the survey observations in the first observing season, the observing strategy and quality of the data(More)
Context. Massive clusters are more often found in actively star forming galaxies than in quiescent ones, similar to the Milky Way. Aims. We have carried out an extensive survey of obscured Milky Way clusters to determine whether our Galaxy is still forming such objects. Methods. Near-infrared spectral classification of some probable cluster members was used(More)
We have surveyed the 30 Myr-old cluster NGC 2547 for planetary debris disks using Spitzer. At 4.5–8 µm we are sensitive to the photospheric level down to mid-M stars (0.2 M ⊙) and at 24 µm to early-G stars (1.2 M ⊙). We find only two to four stars with excesses at 8 µm out of ∼400–500 cluster members, resulting in an excess fraction 1% at this wavelength.(More)
  • J Borissova, V D Ivanov, D Minniti, D Geisler, A W Stephens
  • 2005
This paper is part of a project to search the inner Milky Way for hidden massive clusters and to address the question of whether our Galaxy still forms clusters similar to the progenitors of the present-day globular clusters. We report high angular resolution deep near-infrared imaging of 21 cluster candidates selected from the catalogues of Bica et al.(More)
  • J Borissova, P Pessev, V D Ivanov, I Saviane, R Kurtev, G R Ivanov
  • 2003
Three new obscured Milky Way clusters were detected as surface density peaks in the 2MASS point source catalog during our ongoing search for hidden globular clusters and massive Arches-like star clusters. One more cluster was discovered serendipitously during a visual inspection of the candidates. The first deep J, H, and K s imaging of the cluster [IBP(More)
  • F Mannucci, R Maiolino, G Cresci, M Della Valle, L Vanzi, F Ghinassi +3 others
  • 2002
We report the results of our ongoing search for extincted supernovae (SNe) at near-infrared wavelengths. We have monitored at 2.2µm a sample of 46 Luminous Infrared Galaxies and detected 4 SNe. The number of detections is still small but sufficient to provide the first estimate of supernova rate at near-infrared wavelengths. We measure a SN rate of SN NIR r(More)