Morphology and kinematics of the ionised gas in early-type galaxies

We present results of our ongoing study of the morphology and kinematics of the ionised gas in 48 representative nearby elliptical and lenticular galaxies using the SAURON integral-field spectrograph on the 4.2m William Herschel Telescope. Making use of a recently developed technique, emission is detected in 75% of the galaxies. The ionised-gas distributions display varied morphologies, ranging from regular gas disks to filamentary structures. Additionally, the emission-line kinematic maps show, in general, regular motions with smooth variations in kinematic position angle. In most of the galaxies, the ionised-gas kinematics is decoupled from the stellar counterpart, but only some of them present signatures of recent accretion of gaseous material. The presence of dust is very common in our sample and is usually accompanied by gas emission. Our analysis of the [OIII]/Hbeta emission-line ratios, both across the whole sample as well as within the individual galaxies, suggests that there is no unique mechanism triggering the ionisation of the gas.Comment: 8 pages, 2 figures, submitted to "Adaptive Optics-Assisted Integral-Field Spectroscopy", Rutten R.G.M., Benn C.R., Mendez J., eds., May 2005, La Palma (Spain), New Astr. Rev. For full resolution PS, see http://www.strw.leidenuniv.nl/~jfalcon/JFB_AOmeeting_color_hires.ps.g

Discovery of an old nova remnant in the Galactic globular cluster M 22

A nova is a cataclysmic event on the surface of a white dwarf in a binary system that increases the overall brightness by several orders of magnitude. Although binary systems with a white dwarf are expected to be overabundant in globular clusters (GCs) compared to the Galaxy, only two novae from Galactic globular clusters have been observed. We present the discovery of an emission nebula in the Galactic globular cluster M 22 (NGC 6656) in observations made with the integral-field spectrograph MUSE. We extract the spectrum of the nebula and use the radial velocity determined from the emission lines to confirm that the nebula is part of NGC 6656. Emission-line ratios are used to determine the electron temperature and density. It is estimated to have a mass of 1 to $17 \times 10^{-5}$ solar masses. This mass and the emission-line ratios indicate that the nebula is a nova remnant. Its position coincides with the reported location of a 'guest star', an ancient Chinese term for transients, observed in May 48 BCE. With this discovery, this nova may be one of the oldest confirmed extrasolar events recorded in human history.Comment: 7 pages, 3 figures; accepted for publication in Astronomy & Astrophysic

A young star-forming galaxy at z = 3.5 with an extended Ly\,α\alpha halo seen with MUSE

Spatially resolved studies of high redshift galaxies, an essential insight into galaxy formation processes, have been mostly limited to stacking or unusually bright objects. We present here the study of a typical (L$^{*}$, M$_\star$ = 6 $\times 10^9$ $M_\odot$) young lensed galaxy at $z=3.5$, observed with MUSE, for which we obtain 2D resolved spatial information of Ly$\alpha$ and, for the first time, of CIII] emission. The exceptional signal-to-noise of the data reveals UV emission and absorption lines rarely seen at these redshifts, allowing us to derive important physical properties (T$_e\sim$15600 K, n$_e\sim$300 cm$^{-3}$, covering fraction f$_c\sim0.4$) using multiple diagnostics. Inferred stellar and gas-phase metallicities point towards a low metallicity object (Z$_{\mathrm{stellar}}$ = $\sim$ 0.07 Z$_\odot$ and Z$_{\mathrm{ISM}}$ $<$ 0.16 Z$_\odot$). The Ly$\alpha$ emission extends over $\sim$10 kpc across the galaxy and presents a very uniform spectral profile, showing only a small velocity shift which is unrelated to the intrinsic kinematics of the nebular emission. The Ly$\alpha$ extension is $\sim$4 times larger than the continuum emission, and makes this object comparable to low-mass LAEs at low redshift, and more compact than the Lyman-break galaxies and Ly$\alpha$ emitters usually studied at high redshift. We model the Ly$\alpha$ line and surface brightness profile using a radiative transfer code in an expanding gas shell, finding that this model provides a good description of both observables.Comment: 19 pages, 15 figures, accepted in MNRA

A MUSE map of the central Orion Nebula (M 42)

We present a new integral-field spectroscopic dataset of the central part of the Orion Nebula (M 42), observed with the MUSE instrument at the ESO VLT. We reduced the data with the public MUSE pipeline. The output products are two FITS cubes with a spatial size of ~5.9'x4.9' (corresponding to ~0.76 pc x 0.63 pc) and a contiguous wavelength coverage of 4595...9366 Angstrom, spatially sampled at 0.2". We provide two versions with a sampling of 1.25 Angstrom and 0.85 Angstrom in dispersion direction. Together with variance cubes these files have a size of 75 and 110 GiB on disk. They represent one of the largest integral field mosaics to date in terms of information content. We make them available for use in the community. To validate this dataset, we compare world coordinates, reconstructed magnitudes, velocities, and absolute and relative emission line fluxes to the literature and find excellent agreement. We derive a two-dimensional map of extinction and present de-reddened flux maps of several individual emission lines and of diagnostic line ratios. We estimate physical properties of the Orion Nebula, using the emission line ratios [N II] and [S III] (for the electron temperature $T_e$) and [S II] and [Cl III] (for the electron density $N_e$), and show two-dimensional images of the velocity measured from several bright emission lines.Comment: Resubmitted to A&A after incorporating referee comments; access to full dataset via http://muse-vlt.eu/science/data-release

The SAURON project - XXI : The spatially resolved UV-line strength relations of early-type galaxies

The unexpected rising flux of early-type galaxies at decreasing ultraviolet (UV) wavelengths is a long-standing mystery. One important observational constraint is the correlation between UVoptical colours and Mg2 line strengths found by Burstein et al. The simplest interpretation of this phenomenon is that the UV strength is related to the Mg line strength. Under this assumption, we expect galaxies with larger Mg gradients to have larger UV colour gradients. By combining UV imaging from GALEX, optical imaging from MDM and SAURON integral-field spectroscopy, we investigate the spatially resolved relationships between UV colours and stellar population properties of 34 early-type galaxies from the SAURON survey sample. We find that galaxies with old stellar populations show tight correlations between the far-UV (FUV) colours (FUV -V and FUV - NUV) and the Mg b index, H beta index and metallicity [Z/H]. The equivalent correlations for the Fe5015 index, a-enhancement [a/Fe] and age are present but weaker. We have also derived logarithmic internal radial colour, measured line strength and derived stellar population gradients for each galaxy and again found a strong dependence of the FUV -V and FUV - NUV colour gradients on both the Mg b line strength and the metallicity gradients for galaxies with old stellar populations. In particular, global gradients of Mg b and [Z/H] with respect to the UV colour [e.g. ?(Mg b)/(FUV - NUV) and ?[Z/H]/?(FUV - NUV)] across galaxies are consistent with their local gradients within galaxies, suggesting that the global correlations also hold locally. From a simple model based on multiband colour fits of UV upturn and UV-weak galaxies, we have identified a plausible range of parameters that reproduces the observed radial colour profiles. In these models, the centres of elliptical galaxies, where the UV flux is strong, are enhanced in metals by roughly 60 per cent compared to UV-weak regions.Peer reviewe

Unveiling the counter-rotating nature of the kinematically distinct core in NGC5813 with MUSE

Multi-Unit Spectroscopic Explorer (MUSE) observations of NGC5813 reveal a complex structure in the velocity dispersion map, previously hinted at by SAURON observations. The structure is reminiscent of velocity dispersion maps of galaxies comprising two counter-rotating discs, and might explain the existence of the kinematically distinct core (KDC). Further evidence for two counter-rotating components comes from the analysis of the higher moments of the stellar line-of-sight velocity distributions and fitting MUSE spectra with two separate Gaussian line-of-sight velocity distributions. The emission-line kinematics show evidence of being linked to the present cooling flows and the buoyant cavities seen in X-rays. We detect ionized gas in a nuclear disc-like structure, oriented like the KDC, which is, however, not directly related to the KDC. We build an axisymmetric Schwarzschild dynamical model, which shows that the MUSE kinematics can be reproduced well with two counter-rotating orbit families, characterized by relatively low angular momentum components, but clearly separated in integral phase space and with radially varying contributions. The model indicates that the counter-rotating components in NGC5813 are not thin discs, but dynamically hot structures. Our findings give further evidence that KDCs in massive galaxies should not necessarily be considered as structurally or dynamically decoupled regions, but as the outcomes of the mixing of different orbital families, where the balance in the distribution of mass of the orbital families is crucial. We discuss the formation of the KDC in NGC5813 within the framework of gas accretion, binary mergers and formation of turbulent thick discs from cold streams at high redshif

The Nature of Galactic Bulges from SAURON Absorption Line Strength Maps

We discuss SAURON absorption line strength maps of a sample of 24 early-type spirals, mostly Sa. From the Lick indices H$\beta$, Mg b and Fe 5015 we derive SSP-ages and metallicities. By comparing the scaling relations of Mg b and H beta and central velocity dispersion with the same relation for the edge-on sample of Falcon-Barroso et al. (2002) we derive a picture in which the central regions of Sa galaxies contain at least 2 components: one (or more) thin, disc-like component, often containing recent star formation, and another, elliptical-like component, consisting of old stars and rotating more slowly, dominating the light above the plane. If one defines a bulge to be the component responsible for the light in excess of the outer exponential disc, then many Sa-bulges are dominated by a thin, disc-like component containing recent star formation.Comment: 4 pages, 2 figures, to be published in the proceedings of IAU Symposium No. 241, "Stellar Populations as Building Blocks of Galaxies", editors A. Vazdekis and R.F. Peletie

DIE EINSCHRÄNKUNG DER VERWENDUNG DER GLAGOLIZA AUF DER SYNODE VON ZADAR 1460

U radu se prikazuje odluka Zadarske sinode od 4. prosinca 1460. na kojoj je nadbiskup Mafej Vallaresso pokušao suzbiti upotrebu liturgije na crkvenoslavenskom jeziku hrvatske redakcije (lingua sclava). Sinodalni akti nisu danas sačuvani već je dostupan samo jedan dio sinodalnog kanona u dvije verzije. Originalnu verziju donosi Carlo F. Bianchi, dok je drugu, neznatno izmijenjenu, pribilježio Ivan Zanotti – Tanzlingher. Poslije interpretcije i konzultacije mjerodavnih vrela zaključuje se kako sinodalna odredba nije posve dokidala liturgijska slavlja na hrvatskom jeziku nego je samo na sinodi poduzet pothvat prostornog i vremenskog suzbijanja »glagoljaške liturgije«. Zadarski su nadbiskupi pokušavali tijekom XVI. stoljeća suzbiti glagoljicu na teritoriju nadbiskupije, ali – kako to pokazuju dostupna vrela – nisu imali znatnijeg uspjeha.In this short discussion author analyzes decisions of the Zadar synod that was held on 4th December 1460. At this diocese council archbishop Mafeo Vallaresso tried to suppress local custom of having the holy service in Church-Slavonic language. The acts from this synod unfortunately are not completely preserved but only one article De celebratione missarum et elebrandi divina official today is known in two versions. The first, and presumably original, version was brought to us by Carlo F. Bianchi, and the second one, just slightly modified, was noted by Ivan Zanotti-Tanzlingher. The both notes deliver basically the same information, and differ only regarding the beginning of this act. Archbishop Vallaresso deeply influenced ecclesiastical life of his diocese at his time: he renovated archbishopric palace, ordered a new bell for the cathedral’s bell tower, and restored organ in the cathedral of St. Anastasia. Still, even though he was a typical renaissance man, he did not care much about the specific local tradition of Zadar and deeply rooted Croatian language. Moreover, through the synod he tried to restrain Glagolitic liturgy only to two town churches: St. Donatus (Holy Trinity) and St. Mary the Great. Similarly, a century later, archbishops of the sixteenth century also tried to suppress Glagolitic script in Zadar, for example on the synods of 1566 and 1594. However, in spite of their endeavors, as it is clearly visible from the extant sources, they did not have much success, and Church Slavonic remained an integral part of local liturgy until the reform of the Second Vatican Council.In dieser kleinen Abhandlung wird die synodale Entscheidung über die Einschränkung der Liturgie in der kirchenslavischen Sprache (der kroatischen Redaktion) analysiert. Der venezianische Patrizier und der Erzbischof von Zadar, Maphäus Vallaresso (1450-1496) hat am 4. Dezember 1460 die Synode in Zadar einberufen; ihre Akten oder Entscheidungen sind nicht erhalten, nur ein kleiner Ausschnitt aus dem Kanon »De celebratione missarum et celebrandi divina officia«. Dieser ist heute in zwei Versionen zugänglich, die sich sprachlich nur geringfügig voneinander unterscheiden. Die Originalversion hat schon Carlo F. Bianchi veröffentlicht und die zweite hat Johannes Zanotti – Tanzlingher in seinem Werk Epitome synodorum dioecesis Iadrensis vermerkt. Die synodale Entscheidung versucht die Liturgie in der kirchenslavischen Sprache der kroatischen Redaktion für bestimmte Zeit nur auf zwei Kirchen in Zadar zu reduzieren: Die Kirche der Hl. Dreifaltigkeit (heute hl. Donat) und die Kirche der hl. Maria. Diese Entscheidung ließ sich nicht verwirklichen, da die Liturgie in lingua slava (d. h. in kroatischer Sprache) eine lange Tradition hat und in allen Pfarreien verbreitet war. Die Erzbischöfe von Zadar, Mutius Callinus (1555-1566) und auch Aloysius Molinus (1592-1595) haben diese Entscheidung auf den Synoden 1566 und 1594 noch einmal verbindlich erklärt; die Versuche sind gescheitert. Erzbischof Oktavian Garzzadoro (1623-1644), der aus gesundheitlichen Gründen Papst Urban VIII. um die Entbindung von den Pflichten bat, fügte seiner Begründung hinzu, dass er die Sprache der Gläubigen seines Bistums nicht versteht. Dies ist ein klarer Beweis dafür, dass in Zadar die Bevölkerung kroatisch gesprochen hat und die Liturgie bis zur Reform des II. Vatikanischen Konzils in der Landessprache gefeiert wurde

Bell Correlations and the Common Future

Reichenbach's principle states that in a causal structure, correlations of classical information can stem from a common cause in the common past or a direct influence from one of the events in correlation to the other. The difficulty of explaining Bell correlations through a mechanism in that spirit can be read as questioning either the principle or even its basis: causality. In the former case, the principle can be replaced by its quantum version, accepting as a common cause an entangled state, leaving the phenomenon as mysterious as ever on the classical level (on which, after all, it occurs). If, more radically, the causal structure is questioned in principle, closed space-time curves may become possible that, as is argued in the present note, can give rise to non-local correlations if to-be-correlated pieces of classical information meet in the common future --- which they need to if the correlation is to be detected in the first place. The result is a view resembling Brassard and Raymond-Robichaud's parallel-lives variant of Hermann's and Everett's relative-state formalism, avoiding "multiple realities."Comment: 8 pages, 5 figure