Exploring the correlations between globular cluster populations and supermassive black holes in giant galaxies

This paper presents an analysis of the correlation between the number of globular clusters ($N_{GC}$) in giant galaxies and the mass of the galaxies' central supermassive black hole ( $M_{SMBH}$). I construct a sample of 20 elliptical, spiral, and S0 galaxies with known SMBH masses and with accurately measured GC system properties derived from wide-field imaging studies. The coefficients of the best-fitting $N_{GC}-M_{SMBH}$ relation for the early-type galaxies are consistent with those from previous work but in some cases have smaller relative errors. I examine the correlation between $N_{GC}$ and $M_{SMBH}$ for various subsamples and find that elliptical galaxies show the strongest correlation, while S0 and pseudobulge galaxies exhibit increased scatter. I also compare the quality of the fit of the numbers of metal-poor GCs versus SMBH mass and the corresponding fit for metal-rich GCs. I supplement the 20 galaxy sample with 10 additional galaxies with reliable $N_{GC}$ determinations but without measured $M_{SMBH}$. I use this larger sample to investigate correlations between $N_{GC}$ and host galaxy properties like total galaxy luminosity and stellar mass, and bulge luminosity and mass. I find that the tightest correlation is between $N_{GC}$ and total galaxy stellar mass. This lends support to the notion that $N_{GC}$ and $M_{SMBH}$ are not directly linked but are correlated because both quantities depend on the host galaxy potential. Finally, I use the $N_{GC}-M_{SMBH}$ relation derived from the 20 galaxy sample to calculate predicted $M_{SMBH}$ values for the 10 galaxies with accurate $N_{GC}$ measurements but without measured SMBH masses

Globular cluster systems of spiral and S0 galaxies: Results from WIYN imaging of NGC1023, NGC1055, NGC7332, and NGC7339

We present results from a study of the globular cluster (GC) systems of four spiral and S0 galaxies imaged as part of an ongoing wide-field survey of the GC systems of giant galaxies. The target galaxies - the SB0 galaxy NGC1023, the SBb galaxy NGC1055, and an isolated pair comprised of the Sbc galaxy NGC7339 and the S0 galaxy NGC7332 - were observed in BVR filters with the WIYN 3.5m telescope and Minimosaic camera. For two of the galaxies, we combined the WIYN imaging with previously published data from the $\textit{Hubble Space Telescope}$ and the Keck Observatory to help characterize the GC distribution in the central few kiloparsecs. We determine the radial distribution (surface density of GCs versus projected radius) of each galaxy's GC system and use it to calculate the total number of GCs ($N_{GC}$). We find $N_{GC}$ = 490 ± 30, 210 ± 40, 175 ± 15, and 75 ± 10 for NGC1023, NGC1055, NGC7332, and NGC7339, respectively. We also calculate the GC specific frequency (N GC normalized by host galaxy luminosity or mass) and find values typical of those of the other spiral and E/S0 galaxies in the survey. The two lenticular galaxies have sufficient numbers of GC candidates for us to perform statistical tests for bimodality in the GC color distributions. We find evidence at a high confidence level (>95%) for two populations in the $B - R$ distribution of the GC system of NGC1023. We find weaker evidence for bimodality (>81% confidence) in the GC color distribution of NGC7332. Finally, we identify eight GC candidates that may be associated with the Magellanic dwarf galaxy NGC1023A, which is a satellite of NGC1023

An X-ray emitting black hole in a globular cluster

We present optical and X-ray data for the first object showing strong evidence for being a black hole in a globular cluster. We show the initial X-ray light curve and X-ray spectrum which led to the discovery that this is an extremely bright, highly variable source, and thus must be a black hole. We present the optical spectrum which unambiguously identifies the optical counterpart as a globular cluster, and which shows a strong, broad [O III] emission line, most likely coming from an outflow driven by the accreting source.Comment: 5 pages, 2 figures, to appear in the proceedings of IAUS 246, "Dynamical Evolution of Dense Stellar Systems", ed. Vesperini, Giersz and Sill

A Study of Astaxanthin : Its Application for the Pigmentation of Salmonid Fish

1. The pink-red coloration of the flesh of salmonids is due to carotenoids, especially astaxanthin, and is an important factor to evaluate marketing value of cultured salmonids. For many years fish technologists and scientists have endeavored to enhance the coloration of salmonids through the use of crustacean waste, yeast, algae, flower patels and synthetic carotenoids. 2. Synthetic canthaxanthin and astaxanthin are the two most effecient carotenoids for pigmenting salmonids, and are now widly used in salmonids culture. 3. The metabolism of astaxanthin in salmonids has been studied. The reductive metabolism of astaxanthin to β-carotene have been proposed. The proposed pathways are ; Astaxanthin→idoxanthin→adonixanthin→zeaxanthin, and Canthaxanthin→4-hydroxyechinenone→echinenone→β-carotene. 4. One of well-known functions of carotenoids in fish is pro-vitamin A activity. Salmonid fish are able to convert β-carotene, canthaxanthin, lutein, zeaxanthin and astaxanthin, into vitamin A

Wide-field kinematics of globular clusters in the Leo I group

We present wide-field spectroscopy of globular clusters around the Leo I group galaxies NGC 3379 and NGC 3384 using the FLAMES multi-fibre instrument at the VLT. We obtain accurate radial velocities for 42 globular clusters (GCs) in total, 30 for GCs around the elliptical NGC 3379, eight around the lenticular NGC 3384, and four which may be associated with either galaxy. These data are notable for their large radial range extending from 07 to 145 (2 to 42 kpc) from the centre of NGC 3379, and small velocity uncertainties of about 10 km s-1. We combine our sample of 30 radial velocities for globular clusters around NGC 3379 with 8 additional GC velocities from the literature, and find a projected velocity dispersion of km s-1 at R 5'. These velocity dispersions are consistent with a dark matter halo around NGC 3379 with a concentration in the range expected from a CDM cosmological model and a total mass of 6 . Such a model is also consistent with the stellar velocity dispersion at small radii and the rotation of the ring at large radii, and has a (M/L)B that increases by a factor of five from several kpc to 100 kpc. Our velocity dispersion for the globular cluster system of NGC 3379 is somewhat higher than that found for the planetary nebulae (PNe) in the inner region covered by the PN data, and we discuss possible reasons for this difference. For NGC 3384, we find the GC system has a rotation signature broadly similar to that seen in other kinematic probes of this SB0 galaxy. This suggests that significant rotation may not be unusual in the GC systems of disc galaxies

The globular cluster system in the outer regions of NGC 4472

Accepted for publication in The Astronomical Journal, January 2001 issueConsiglio Nazionale delle Ricerche - Biblioteca Centrale - P.le Aldo Moro, 7 Rome; International School for Advanced Studies, Via Beirut, 7 Trieste / CNR - Consiglio Nazionale delle RichercheSIGLEITItal

The rise and fall of Lake Bonneville between 45 and 10.5 ka

A sediment core taken from the western edge of the Bonneville Basin has provided high-resolution proxy records of relative lake-size change for the period 45.1-10.5 calendar ka (hereafter ka). Age control was provided by a paleomagnetic secular variation (PSV)-based age model for Blue Lake core BL04-4. Continuous records of δ18O and total inorganic carbon (TIC) generally match an earlier lake-level envelope based on outcrops and geomorphic features, but with differences in the timing of some hydrologic events/states. The Stansbury Oscillation was found to consist of two oscillations centered on 25 and 24 ka. Lake Bonneville appears to have reached its geomorphic highstand and began spilling at 18.5 ka. The fall from the highstand to the Provo level occurred at 17.0 ka and the lake intermittently overflowed at the Provo level until 15.2 ka, at which time the lake fell again, bottoming out at ~14.7 ka. The lake also fell briefly below the Provo level at ~15.9 ka. Carbonate and δ18O data indicate that between 14.7 and 13.1 ka the lake slowly rose to the Gilbert shoreline and remained at about that elevation until 11.6 ka, when it fell again. Chemical and sedimentological data indicate that a marsh formed in the Blue Lake area at 10.5 ka. Relatively dry periods in the BL04-4 records are associated with Heinrich events H1eH4, suggesting that either the warming that closely followed a Heinrich event increased the evaporation rate in the Bonneville Basin and (or) that the core of the polar jet stream (PJS) shifted north of the Bonneville Basin in response to massive losses of ice from the Laurentide Ice Sheet (LIS) during the Heinrich event. The second Stansbury Oscillation occurred during Heinrich event H2, and the Gilbert wet event occurred during the Younger Dryas cold interval. Several relatively wet events in BL04-4 occur during Dansgaard- Oeschger (DO) warm events. The growth of the Bear River glacier between 32 and 17 ka paralleled changes in the values of proxy indicators of Bonneville Basin wetness and terminal moraines on the western side of the Wasatch Mountains have ages ranging from 16.9 to 15.2 ka. This suggests a near synchroneity of change in the hydrologic and cryologic balances occurring in the Bonneville drainage system and that glacial extent was linked to lake size

Dietary effects on the reproductive performance of the sea urchin Tripneustes gratilla ll: Implications for offspring performance

Aquaculture practices can result in declines in the genetic diversity observed in progenitor natural populations, resulting in subsequent poor production output, particularly for broadcast spawning animals that frequently display differential parental contributions. This study aimed to assess the effect of different Tripneustes gratilla broodstock feeding regimes [formulated feed, kelp (Ecklonia maxima), green seaweed (Ulva lacinulata) and mixture of the three diets for four months] on larval growth, parental contributions and juvenile performance after a factorial breeding design was implemented. Larvae produced from broodstock fed kelp and the mixed diet survived for the full duration of larval rearing and displayed similar growth rates throughout (p > 0.05). Though larvae from Ulva-fed broodstock did not survive for the full duration of larval rearing, this could have been a consequence of larval rearing practices, as these larvae displayed a rapid increase in post-oral arm lengths prior to the mortality event. Furthermore, these larvae survived for the longest amount of time when left unfed, suggesting that the maternal reserves from animals fed Ulva as a broodstock conditioning diet could be beneficial to development in early larval stages. In contrast, larvae from animals fed a formulated feed did not survive the full duration of larval rearing and had developmental abnormalities. Three months post-metamorphosis, 10 species-specific microsatellite markers were PCR amplified across 16 broodstock and 364 offspring from kelp and mixed diet fed animals. Genetic diversity analyses showed that there were no statistically significant (p > 0.05) differences between the broodstock animals and their offspring, showing that factorial breeding designs are advantageous to preserve genetic diversity present in cultured cohorts. Parentage analyses revealed that a total of 26 out of 32 possible F1 parent pairs contributed to the F2 generation, with a low heritability estimate of approximately zero (0.050 ± 0.058) for offspring body diameter, likely as offspring phenotypic performance is not influenced by additive genetic effects during these early growth stages