Temperatures and metallicities of M giants in the galactic Bulge from low-resolution K-band spectra

With the existing and upcoming large multi-fibre low-resolution spectrographs, the question arises how precise stellar parameters such as Teff and [Fe/H] can be obtained from low-resolution K-band spectra with respect to traditional photometric temperature measurements. Until now, most of the effective temperatures in galactic Bulge studies come directly from photometric techniques. Uncertainties in interstellar reddening and in the assumed extinction law could lead to large systematic errors. We aim to obtain and calibrate the relation between Teff and the $\rm ^{12}CO$ first overtone bands for M giants in the galactic Bulge covering a wide range in metallicity. We use low-resolution spectra for 20 M giants with well-studied parameters from photometric measurements covering the temperature range 3200 < Teff < 4500 K and a metallicity range from 0.5 dex down to -1.2 dex and study the behaviour of Teff and [Fe/H] on the spectral indices. We find a tight relation between Teff and the $\rm ^{12}CO(2-0)$ band with a dispersion of 95 K as well as between Teff and the $\rm ^{12}CO(3-1)$ with a dispersion of 120 K. We do not find any dependence of these relations on the metallicity of the star, making them relation attractive for galactic Bulge studies. This relation is also not sensitive to the spectral resolution allowing to apply this relation in a more general way. We also found a correlation between the combination of the NaI, CaI and the $\rm ^{12}CO$ band with the metallicity of the star. However this relation is only valid for sub-solar metallicities. We show that low-resolution spectra provide a powerful tool to obtain effective temperatures of M giants. We show that this relation does not depend on the metallicity of the star within the investigated range and is also applicable to different spectral resolution.Comment: 6 pages, accepted for publication in Astronomy&Astrophysic

M Giants with IGRINS II. Chemical Evolution of Fluorine at High Metallicities

The origin and evolution of fluorine in the Milky Way galaxy is still in debate. In particular, the increase of the [F/Fe] in metal-rich stars found from near-IR HF-lines is challenging to explain theoretically. We determine the fluorine abundances from 50 M giants in the solar neighbourhood spanning a broad range of metallicities (-0.9<[Fe/H]<0.25 dex). These stars are cool enough to have an array of HF lines in the K band. We observed the stars with the IGRINS and investigate each of ten HF molecular lines in detail. Based on a detailed line-by-line analysis of ten HF lines, we find that the R19, R18 and R16 lines should primarily be used for abundance analysis. The R15, R14 and R13 lines can also be used, but the trends based on these lines show increasing dependencies with the stellar parameters. The strongest HF lines, namely R12, R11, R9 and R7 should be avoided since the abundances from them show significant trends with the stellar parameters, and a high sensitivity to variations in the microturbulence, especially for coolest metal-rich stars. This leads to a huge scatter and high fluorine abundances for supersolar metallicity stars, not seen in the trends from the weaker lines for the same stars. When estimating the final mean fluorine abundance trend versus metallicity, we neglect the fluorine abundances from the four strongest lines (R7, R9, R11 and R12) for all stars and use only those derived from R16, R18, and R19 for the coolest metal-rich stars. We confirm the flat trend of [F/Fe] found in other studies in the metallicity range of -1.0<[Fe/H]<0.0. We also find a slight enhancement at supersolar metallicities (0<[Fe/H]<0.15) but we cannot confirm the upward trend seen at [Fe/H]>0.25. We need more observations of M giants at super solar metallicities with a spectrometer like IGRINS to confirm if the metal-rich fluorine abundance upturn is real or not.Comment: 11 pages, 6 figures, Accepted for publication in A&

Generation of Test Vectors for Sequential Cell Verification

For Application Specific Integrated Circuits (ASIC) and System-on-Chip (SOC) designs, Cell - Based Design (CBD) is the most prevalent practice as it guarantees a shorter design cycle, minimizes errors and is easier to maintain. In modern ASIC design, standard cell methodology is practiced with sizable libraries of cells, each containing multiple implementations of the same logic functionality, in order to give the designer differing options based on area, speed or power consumption. For such library cells, thorough verification of functionality and timing is crucial for the overall success of the chip, as even a small error can prove fatal due to the repeated use of the cell in the design. Both formal and simulation based methods are being used in the industry for cell verification. We propose a method using the latter approach that generates an optimized set of test vectors for verification of sequential cells, which are guaranteed to give complete Single Input Change transition coverage with minimal redundancy. Knowledge of the cell functionality by means of the State Table is the only prerequisite of this procedure

Innovative exploitation of deepsea crustaceans along the Kerala coast

Exploratory surveys carried out since 1965 by fishing vessels belonging to different governmental agencies have revealed the occurrence of commercially Important deep sea crustaceans in trawlable concentration along the south-west coast of India

The "karikkadi" fishery of Kerala

Parapenaeopsis stylifera, (called 'Karikkadi Chemmeen' ) is the most important species of prawn contributing to the commercial fishery of Kerala coast. An experimental shrimp trawling conducted for a period of two years has shown that during the non-monsoon period (September/October to May) most of the shrimp stocks occupy the coastal waters within the 20 m depth contour. With the commencement of southwest monsoon and the consequent changes in the environmental conditions, the prawns leave the inshore areas in large numbers to the deeper zones. The wide annual fluctuations observed at important centres, the occurrence of juvenile prawns in large quantities noticed quite often in the fishery, call for proper management and conservation measures

Observations on the prawn fishery off Sakthikulangara in the light of monsoon trawling ban

Sakthikulangara is the most important prawn landing center in Kerala. Study on the prawn fishery exploited by shrimp trawlers for a period of 15 years during 1986-200b at rnis centre indicated a decline in the landings in the first five year period followed by improved fishery between 1991 and 1995. However, decline in catch and catch rate was registered in the next 5 years. Contribution of Sakthikulangara to the Kerala prawn fishery declined from 51% in seventies to 30% in eighties and 24% in nineties. 'Karikkadi' (Parapenaeopsis stylifera) contributed to 68% of the average annual production during 1986 - 2000. Extension of trawling to middle shelf waters and introduction of night trawling transformed the complexion of prawn fishery in the nineties with the addition of nonconventional species such as Trachypenaeus curuirostris, Solenocera choprai and Penaeus canaliculatus. Analysis of data on prawn fishery at Sakthikulangara for a period of 20 years (1981-2000) to study the impact of ban on monsoon trawling has indicated that trawling ban for a short duration of 45 days in the first half of the season is advantageous to the 'Karikkadi' fishery

Is the deep sea prawn fishery of Kerala sustainable?

The enterprising small and medium shrimp trawler operators of Kerala ventured into deep sea fishing for the first time in November 1999 defying the longheld concept that deep sea prawn resources could be harvested only by means of large trawlers. This endeavour proved successful with the realisation of 25,647 t of deep sea prawns in the first fishing season lasting between November '99 and May 2000

Consultancy services in marine fisheries- A profile of technologies and experts

The ICAR system currently needs very effective partnership between the researchers and the user groups. The Central Marine Fisheries Research Institute, a premier Institute under the ICAR, has taken effective steps to introduce the services and technologies in the marine fisheries sector, achieved over the last 50 years R & D activities. With a viev/ to institutionalising transfer of technologies, the institute has constituted a Consultancy Processing Cell (CPC) in 1997 for effectively serving the needs of our clients, through the short term and long term trainings, consultancies, contract services and contract research

Larval development of Metapenaeus moyebi (Kishinouye) reared in the laboratory

The complete larval development of Metapenaeus moyebi was studied by rearing them in the CMFRI laboratory at Karwar. The viable eggs take 8i to 10 hours to hatch out and the duration of nauplius stage ranges between 37 and 44 hours. The protozoea transforms into mysis after 5 to 5i days. The mysis stage lasts for 91/2 to lO1/2 days. Complete larval development from egg to postlarva I takes 16-181 days. There are 6 nauplius sub-stages, 3 protozoea substages, 3 mysis substages and 1 intermediate stage during the course of development. The detailed structure of the larval substages is described and illustrated in this paper

Detailed α\alpha abundance trends in the inner Galactic bulge

In this paper, we aim to derive high-precision alpha-element abundances using CRIRES high-resolution IR spectra of 72 cool M giants of the inner Galactic bulge. Silicon, magnesium, and calcium abundances were determined by fitting a synthetic spectrum for each star. We also incorporated recent theoretical data into our spectroscopic analysis (i.e. updated K-band line list, better broadening parameter estimation, non-local thermodynamic equilibrium (NLTE) corrections). We compare these inner bulge alpha abundance trends with those of solar neighbourhood stars observed with IGRINS using the same line list and analysis technique; we also compare our sample to APOGEE DR17 abundances for inner bulge stars. We investigate bulge membership using spectro-photometric distances and orbital simulations. We construct a chemical-evolution model that fits our metallicity distribution function (MDF) and our alpha-element trends. Among our 72 stars, we find four that are not bulge members. [Si/Fe] and [Mg/Fe] versus [Fe/H] trends show a typical thick disc alpha-element behaviour, except that we do not see any plateau at supersolar metallicities as seen in other works. The NLTE analysis lowers [Mg/Fe] typically by $\sim$0.1 dex, resulting in a noticeably lower trend of [Mg/Fe] versus [Fe/H]. The derived [Ca/Fe] versus [Fe/H] trend has a larger scatter than those for Si and Mg, but is in excellent agreement with local thin and thick disc trends. With our updated analysis, we constructed one of the most detailed studies of the alpha abundance trends of cool M giants in the inner Galactic bulge. We modelled these abundances by adopting a two-infall chemical-evolution model with two distinct gas-infall episodes with timescales of 0.4 Gyr and 2 Gyr, respectively. Based on a very meticulous spectral analysis, we have constructed detailed and precise chemical abundances of Mg, Si, and Ca for cool M giants.Comment: 19 pages, 11 figure