arXiv subjects

Alberto Franceschini

Publications and source records attributed to Alberto Franceschini.

49 records · Page 3Linked to original sources

arXiv2002

The LARI Method for ISO-CAM/PHOT Data Reduction and Analysis

The techniques and software tools developed for the reduction and analysis of ISO-CAM/PHOT data with the LARI method are presented. The method, designed for the detection of faint sources in ISO raster observations, is based on the assumption of the existence of two different time scales in the detectors' transient behaviour, accounting either for fast or slow detectors' response. The specifically developed IDL software includes: a reduction pipeline performing basic operations such as deglitching and background determination; the fitting procedures proper, modelling the time history of individual pixels and detecting any flux excess with respect to the local background ascribable to potential sources; mapping, source extraction and flux estimation procedures; simulation procedures allowing one to estimate the errors arising from different instrumental and reduction effects. Moreover, an easy-to-use graphical user interface allows one to quickly browse the data and carry out the substantial amount of interactive analysis required when the automatic fit fails and to check the reliability of detected sources. This method provides source lists of great reliability and completeness and an outstanding photometric accuracy, particularly at low redundancy levels, where the reliability of ISO-CAM/PHOT source lists, even at moderately bright flux levels, has been a long-standing issue. In this work a description of the techniques and software tools that have been developed is given, alongside with some highlights from the results obtained thanks to their application to different fields.

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arXiv2002

The SWIRE SIRTF Legacy Program: Studying the Evolutionary Mass Function and Clustering of Galaxies

The SIRTF Wide-area Infrared Extragalactic (SWIRE) survey is a "Legacy Program" using 851 hours of SIRTF observing time to conduct a set of large-area (67 sq. deg. split into 7 fields) high Galactic latitude imaging surveys, achieving 5-sigma sensitivities of 0.45/2.75/17.5 mJy at 24/70/160 micron with MIPS and of 7.3/9.7/27.5/32.5 microJy at 3.6/4.5/5.8/8.0 micron with IRAC. These data will yield highly uniform source catalogs and high-resolution calibrated images, providing an unprecedented view of the universe on co-moving scales up to several hundreds Mpc and to substantial cosmological depths (z\simeq 2.5 for luminous sources). SWIRE will, for the first time, study evolved stellar systems (from IRAC data) versus active star-forming systems and AGNs (from MIPS data) in the same volume, generating catalogues with of order of 2 million infrared-selected galaxies. These fields will have extensive data at other wavebands, particularly in the optical, near-IR and X-rays. SWIRE will provide a complement to smaller and deeper observations in the SIRTF Guaranteed Time and the Legacy Program GOODS, by allowing the investigation of the effect of environment on galaxy evolution. We expand here on capabilities of SWIRE to study with IRAC the evolution of the bright end of the galaxy mass function as a function of cosmic time.

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arXiv2001

The AGN contribution to mid-infrared surveys

We provide constraints on the AGN contribution to the mid-IR extragalactic background light from a correlation analysis of deep X-ray and mid-IR observations in two regions centred on the Lockman Hole (LH) and Hubble Deep Field North (HDFN). Among the 76 galaxies detected by XMM in the LH area (200 square arcminutes), 24 show mid-IR emission, but the relative percentage of X-ray sources with mid-IR counterparts increases with the band energy: from 30% of the 0.5-2 keV sources up to 63% of the 5-10 keV sources. In contrast, only a small fraction of the mid-IR sources (around 10%) show X-ray emission. In the region centred on the HDFN (24 square arcminutes), 25% of the mid-IR sources are detected in the X-ray, while 30-40% of the X-ray sources show mid-IR emission. Under the conservative assumption that all XMM sources are AGN-dominated, AGNs contribute 15% of the total mid-IR flux in the LH. For the HDFN we have assumed that AGN-dominated sources are luminous X-ray sources with radio to X-ray SEDs typical of local AGNs, in which case we find that 18% of the mid-IR flux are due to AGN emission. If we put together all the existing information from the deepest HDFN data to the shallow large-area BeppoSAX observations in the ELAIS S1 region using the median mid-IR to X-ray spectral indices as a function of the X-ray flux, we find an AGN contribution to the 15um background of 17%. We conclude that the population of IR luminous galaxies detected in the ISOCAM deep surveys are mainly constituted by dust-obscured starbursts.

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arXiv2001

ISO investigates the nature of extremely-red hard X-ray sources responsible for the X-ray background

We analyse very deep X-ray and mid-IR surveys in common areas of the Lockman Hole and the HDF North to study the sources of the X-ray background (XRB) and to test the standard obscured accretion paradigm. We detect with ISO a rich population of X-ray luminous sources with red optical colours, including a fraction identified with Extremely Red Objects (R-K > 5) and galaxies with SEDs typical of normal massive ellipticals or spirals at z ~ 1. The high 0.5-10 keV X-ray luminosities of these objects (1E43-1E45 erg/s) indicate that the ultimate energy source is gravitational accretion, while the X-ray to IR flux ratios and the X-ray spectral hardness show evidence of photoelectric absorption at low X-ray energies. An important hint on the physics comes from the mid-IR data at 6.7 and 15 um, well reproduced by model spectra of completely obscured quasars under standard assumptions and l.o.s. optical depths tau ~ 30-40. Other predictions of the standard XRB picture, like the distributions of intrinsic bolometric luminosities and the relative fractions of type-I and -II objects (1:3), are also consistent with our results. Obscured gravitational accretion is then confirmed as being responsible for the bulk of the X-ray background, since we detect in the IR the down-graded energy photoelectrically absorbed in X-rays: 63% of the faint 5-10 keV XMM sources are detected in the mid-IR by Fadda et al. (2001). However, although as much as 90% of the X-ray energy production could be converted to IR photons, no more than 20% of the Cosmic IR Background can be attributed to X-ray loud AGNs.

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arXiv2000

Star Formation and Selective Dust Extinction in Luminous Starburst Galaxies

We investigate the star formation and dust extinction properties of very luminous infrared galaxies whose spectra display a strong Hdelta line in absorption and a moderate [OII] emission (e[a] spectrum). This spectral combination has been suggested to be a useful method to identify dusty starburst galaxies at any redshift on the basis of optical data alone. We compare the average e(a) optical spectrum with synthetic spectra that include both the stellar and the nebular contribution, allowing dust extinction to affect differentially the stellar populations of different ages. We find that reproducing the e(a) spectrum requires the youngest stellar generations to be significantly more extinguished by dust than older stellar populations, and implies a strong ongoing star formation activity at a level higher than in quiescent spirals. A model fitting the optical spectrum does not necessarily produce the observed FIR luminosity and this can be explained by the existence of stellar populations which are practically obscured at optical wavelengths. Models in which dust and stars are uniformly mixed yield a reddening of the emerging emission lines which is too low compared to observations: additional foreground reddening is required.

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arXiv2000

High-Redshift Galaxies: The Far-Infrared and Sub-Millimeter View

Observations at long wavelengths, in the wide interval from a few to 1000 micron, are essential to study diffuse media in galaxies, including all kinds of atomic, ionic and molecular gases and dust grains. Hence they are particularly suited to investigate the early phases in galaxy evolution, when a very rich ISM is present in the forming systems. During the last few years a variety of observational campaigns in the far-IR/sub-mm, exploiting both ground-based and space instrumentation, have started to provide results of relevant cosmological impact. Most crucial among these have been the discovery of an intense diffuse background in the far-IR/sub-mm of extragalactic origin, and the deep explorations from space in the far-IR and with large millimetric telescopes on ground. These results challenge those obtained from optical-UV observations, by revealing luminous to very luminous phases in galaxy evolution at substantial redshifts, likely corresponding to violent events of star-formation in massive systems. This is bringing to significant refinements of the present schemes of galaxy formation, as far as the history of baryon transformations is concerned.

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arXiv1999

On the Relationship between Galaxy Formation and Quasar Evolution

We compare the evolution with cosmic time of the star-formation rate per comoving volume in galaxies and of the volume emissivity by Active Galactic Nuclei, as a clue to understand the relationship between black hole accretion and the formation of the surrounding structure. We find an interesting similarity between the evolution rates for the total populations of galaxies and AGNs, which indicates that, on average, the history of BH accretion tracks that of stellar formation in the hosting galaxies. Similarly, the evolution of luminous quasars parallels that of the stellar populations in massive spheroidal galaxies, in keeping with the locally established association of supermassive BHs and galactic bulges. We finally comment on our finding that high-luminosity, high-mass systems evolve on a faster cosmic timescale than the lower mass ones: to explain this, the theories of structure formation based on the gravitational collapse of dark matter halos have to be complemented with a detailed description of the dynamical processes in the baryonic component, which dominate the formation and evolution in high-density environments.

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arXiv1999

Dust Emission from Quasars and Quasar Host Galaxies

We test emission models of circum-nuclear dust torii around quasars, at low and high redshifts, by using a large collection of photometric data for an unbiased sample of 120 optically-selected objects with millimetric and sub-millimetric fluxes, including new unpublished data. Under the assumption that the dust is heated by a point-like source with a power-law primary spectrum, as defined by the observed optical-UV continuum, we infer the basic model parameters, such as dust masses, temperature distributions and torus sizes, by numerically solving the radiative transfer equation in the dust distribution. In addition to the substantiated statistics, an essential improvement over previous analyses comes from the use of optical-UV data to constrain the primary illuminating continuum, which is needed to estimate dust temperatures and sizes. Dependences of the best-fit parameters on luminosity and redshift are studied and the contribution of dust in the host galaxy to the observed fluxes is briefly mentioned. This analysis constrains the properties of the enriched interstellar medium in the galaxies hosting the quasars. The dust abundance does not display appreciable trends as a function of redshift, from z ~ 1 to almost 5, and shows that dust and metals are at least as, and often more, abundant at these early epochs than they are in local galactic counterparts. This evolutionary pattern is remarkably at variance with respect to what is expected for disk galaxies, like the Milky Way, slowly building metals during the whole Hubble time. It rather points in favour of a much more active phase of star-formation at early epochs, probably related to the formation of massive spheroidal galaxies.

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arXiv1997

Constraints on the Extragalactic Infrared Background from Gamma Ray Observations of Mrk 501

We use the new results of the HEGRA detector on the TeV gamma-ray emission from MKN 501 to set upper limits on the energy density of the cosmic infrared background (CIRB). Contrary to previous interpretations of the gamma-ray spectrum of MKN 421 as showing an intergalactic absorption cutoff at 5 TeV, the observed spectrum of MKN 501 extends beyond 10 TeV and appears to be unattenuated by gamma-gamma collisions with the low-energy CIRB photons. The upper limits on the CIRB intensity -- derived both assuming an `a priori' shape for the CIRB spectrum and without model-dependent assumptions -- are thus quite strong and come almost in conflict with the observational evaluations based on deep surveys of extragalactic sources in the near- and mid-IR. If spectra at TeV energies for extragalactic gamma-ray sources like this for MKN 501 will be confirmed with improved statistics, we may be forced to conclude that the process of gamma-gamma interaction in the intergalactic space is more complex than expected and the average intergalactic magnetic field extremely weak.

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arXiv1997

Models of Galaxy Evolution from the UV to the Sub-Millimeter

We present the first results of a detailed modeling of chemical and photometric evolution of galaxies including the effects of a dusty interstellar medium. A chemical evolution code follows the SF rate, the gas fraction and the metallicity, basic ingredients for the stellar population synthesis. The latter is performed with a grid of integrated spectra for SSP of different ages and metallicities, in which the effects of dusty envelopes around AGB stellar are included. The residual fraction of gas in the galaxy is divided into two phases: the star forming molecular clouds and the diffuse medium. The molecular gas is sub-divided into clouds of given mass and radius: it is supposed that any SSP is borne within the cloud and progressively escapes it. The emitted spectrum of the star forming molecular clouds is computed with a radiative transfer code. The diffuse dust emission (cirrus) is derived by describing the galaxy as an axially symmetric system, in which the local dust emissivity is consistently calculated as a function of the local field intensity due to the stellar component. Effects of very small grains, subject to temperature fluctuations, as well as PAH are included. The model is compared and calibrated with available data of starburst galaxies in the local universe, in particular new broad-band and spectroscopic ISO observations. It will be a fundamental tool to extract information on global evolution of the stellar component and of ISM of galaxies from observations covering four decades in $λ$. The combination of observations from HST, Keck, ISO and ground-based optical, IR and sub-mm telescopes already provided several objects at relevant $z$ with spectral information on this large $λ$ range. Their number will increase after the completion of ISO surveys, and will burst when SIRFT, FIRST, Planck

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arXiv1997

Old Massive Ellipticals and S0 in the Hubble Deep Field Vanish from View at $z>1.3$: Possible Solutions of the Enigma

We have investigated the properties of a bright K-band selected sample of early-type galaxies in the Hubble Deep Field, as representative of the field galaxy population. This dataset is unique as for the morphological information on faint high-z sources, and for complete photometric and spectroscopic coverage. The majority of bright early-type galaxies in this field are found at redshifts $z \leq 1.3$ to share common properties with those of high-z cluster samples, as for the age and mass of the dominant stellar population -- which are found to be as old as 3-5 Gyr and as massive as $10^{11} M_\odot$ already at $z\simeq 1$. There is no evidence of a steepening of the mass function from $z$=0 to $z$=1, as inferred by some authors from analyses of optically-selected samples and favoured by hierarchical clustering models forming most of the E/S0s at $z<1$. What distinguishes this sample is a remarkable absence of objects at $z>1.3$, which would be expected as clearly detectable above the flux limits, given the aged properties of the lower redshift counterparts. So, something hide them at high redshifts. Merging could be an explanation, but it would require that already formed and old stellar systems would assemble on short timescales of 1 Gyr or less. Only a negligible fraction of the galactic mass in young stars has to be added, a rather contrived situation from the dynamical point of view. An alternative interpretation could be that a dust-polluted ISM obscures the first 3 to 4 Gyr of the evolution of these massive systems, after which a galactic wind and gas consumption makes them transparent. The presence of dust would have relevant (and testable) implications for the evaluation of the global energetics from galaxy formation and for the visibility of the early phases by current and future infrared

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arXiv1997

Thick tori around AGN: the case for extended tori and consequences for their X-ray and IR emission

Two families of models of dusty tori in AGNs (moderately thick and extended versus very thick and compact) are tested against available observations. The confrontation suggests that the former class better explains the IR broad-band spectra of both broad and narrow line AGNs, the anisotropy of the emission deduced by comparing IR properties of Seyfert 1 and 2 nuclei, the results of IR spectroscopy and those of high spatial resolution observations. There is however clear evidence for a broad distribution of optical depths. We also examine the relationship between IR and X-ray emission. The data support a view in which the matter responsible for the X-ray absorption is mostly dust free, lying inside the dust sublimation radius. The consequences of these results for the hard X-ray background as well as IR counts and background are discussed.

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arXiv1996

Dust Enshrouded AGN Models for Hyperluminous High Redshift IR Galaxies

We investigate models for the power supply and broad-band spectral energy distribution (SED) of hyperluminous IR galaxies, recently discovered at high redshifts, in terms of the emission from an active nucleus embedded in a torus-like dusty structure. We find consistent solutions in terms of a simple torus model extended several hundreds of parsecs, with $A_V$ in the equatorial plane of a few hundreds and a typical covering factor of over $50\%$. Objects as different as the prototype high-z galaxy \fd, the z=0.93 IR object \fq, \fz\ found in a high-z cooling flow, and the optically selected BAL "Cloverleaf" quasar, are all fitted by the same solution, for decreasing values of the polar angle to the line-of-sight and proper scaling of the luminosities. We suggest that such luminous high-z IR objects are heavily buried quasars surrounded by large amounts of dust with high covering factors and large optical depths. Comparison with UVX QSOs suggests that they are observed during a transient phase. Forthcoming observations in the far-IR will soon allow probing this phase and its relationship with the -- possibly concomitant -- formation of the nuclear black hole and of the host galaxy.

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