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Unveiling the nature of INTEGRAL objects through optical spectroscopy. IV. A study of six new hard X-ray sources
We present further results from our onging optical spectrophotometriccampaign at the Astronomical Observatory of Bologna in Loiano (Italy) onunidentified hard X-ray sources detected by INTEGRAL. We observedspectroscopically the putative optical counterparts of the INTEGRALsources IGR J00234+6141, IGR J01583+6713, IGR J06074+2205, IGRJ13091+1137 and IGR J20286+2544. We find that the first two are Galacticobjects, namely a Cataclysmic Variable at a distance d 300 pc anda Be/X transient High-Mass X-ray Binary (HMXB) located at ~6.4 kpc,respectively, whereas the last one is identified with MCG +04-48-002, aStarburst/H ii galaxy at redshift z = 0.013 hiding a Seyfert 2 nucleus.We identify IGR J13091+1137 as the (likely Seyfert 2 type) activenucleus of galaxy NGC 4992, which we classify as an X-ray Bright,Optically Normal Galaxy; this is the first example of this type ofobject to be detected by INTEGRAL, and one of the closest of this class.We moreover confirm the possible Be/X nature of IGR J06074+2205, and weestimate it to be at a distance of ~1 kpc. We also reexamine thespectrum of the z = 0.087 elliptical radio galaxy PKS 0352-686, thepossible counterpart of the INTEGRAL source IGR J03532-6829, and we findthat it is a BL Lac. Physical parameters for these sources are alsoevaluated by discussing our findings in the context of the availablemultiwavelength information. These identifications further stress theimportance of INTEGRAL in the study of the hard X-ray spectrum of ActiveGalactic Nuclei, HMXBs and Cataclysmic Variables.
| EGRET Upper Limits and Stacking Searches of Gamma-Ray Observations of Luminous and Ultraluminous Infrared Galaxies
We present a stacking analysis of EGRET γ-ray observations at thepositions of luminous and ultraluminous infrared galaxies. The latterwere selected from the recently presented HCN survey, which is thoughtto contain the most active star-forming regions of the universe.Different sorting criteria are used, and since there is no positivecollective detection of γ-ray emission from these objects, wedetermined both collective and individual upper limits. The uppermostexcess we find appears in the case of ULIRGs ordered by redshift, at avalue of 1.8 σ.
| HCN Survey of Normal Spiral, Infrared-luminous, and Ultraluminous Galaxies
We report systematic HCN J=1-0 (and CO) observations of a sample of 53infrared (IR) and/or CO-bright and/or luminous galaxies, including sevenultraluminous infrared galaxies, nearly 20 luminous infrared galaxies,and more than a dozen of the nearest normal spiral galaxies. This is thelargest and most sensitive HCN survey of galaxies to date. All galaxiesobserved so far follow the tight correlation between the IR luminosityLIR and the HCN luminosity LHCN initially proposedby Solomon, Downes, & Radford, which is detailed in a companionpaper. We also address here the issue of HCN excitation. There is noparticularly strong correlation between LHCN and the 12 μmluminosity; in fact, of all the four IRAS bands, the 12 μm luminosityhas the weakest correlation with the HCN luminosity. There is also noevidence of stronger HCN emission or a higher ratio of HCN and COluminosities LHCN/LCO for galaxies with excess 12μm emission. This result implies that mid-IR radiative pumping, orpopulating, of the J=1 level of HCN by a mid-IR vibrational transitionis not important compared with the collisional excitation by densemolecular hydrogen. Furthermore, large velocity gradient calculationsjustify the use of HCN J=1-0 emission as a tracer of high-densitymolecular gas (>~3×104/τcm-3) andgive an estimate of the mass of dense molecular gas from HCNobservations. Therefore, LHCN may be used as a measure of thetotal mass of dense molecular gas, and the luminosity ratioLHCN/LCO may indicate the fraction of moleculargas that is dense.
| The Star Formation Rate and Dense Molecular Gas in Galaxies
HCN luminosity is a tracer of dense molecular gas,n(H2)>~3×104cm-3, associatedwith star-forming giant molecular cloud (GMC) cores. We present theresults and analysis of our survey of HCN emission from 65 infraredgalaxies, including nine ultraluminous infrared galaxies (ULIGs,LIR>~1012Lsolar), 22 luminousinfrared galaxies (LIGs,1011Lsolar0.06 are LIGs or ULIGs. Normal spiralsall have similar and low dense gas fractionsLHCN/LCO=0.02-0.05. The global star formationefficiency depends on the fraction of the molecular gas in a densephase.
| An IRAS High Resolution Image Restoration (HIRES) Atlas of All Interacting Galaxies in the IRAS Revised Bright Galaxy Sample
The importance of far-infrared observations for our understanding ofextreme activity in interacting and merging galaxies has beenillustrated by many studies. Even though two decades have passed sinceits launch, the most complete all-sky survey to date from which far-IRselected galaxy samples can be chosen is still that of the InfraredAstronomical Satellite (IRAS). However, the spatial resolution of theIRAS all-sky survey is insufficient to resolve the emission fromindividual galaxies in most interacting galaxy pairs, and hence previousstudies of their far-IR properties have had to concentrate either onglobal system properties or on the properties of very widely separatedand weakly interacting pairs. Using the HIRES image reconstructiontechnique, it is possible to achieve a spatial resolution ranging from30" to 1.5m (depending on wavelength and detector coverage), whichis a fourfold improvement over the normal resolution of IRAS. This issufficient to resolve the far-IR emission from the individual galaxiesin many interacting systems detected by IRAS, which is very importantfor meaningful comparisons with single, isolated galaxies. We presenthigh-resolution 12, 25, 60, and 100 μm images of 106 interactinggalaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS,Sanders et al.), a complete sample of all galaxies having a 60 μmflux density greater than 5.24 Jy. These systems were selected to haveat least two distinguishable galaxies separated by less than threeaverage galactic diameters, and thus we have excluded very widelyseparated systems and very advanced mergers. Additionally, some systemshave been included that are more than three galactic diameters apart,yet have separations less than 4' and are thus likely to suffer fromconfusion in the RBGS. The new complete survey has the same propertiesas the prototype survey of Surace et al. We find no increased tendencyfor infrared-bright galaxies to be associated with other infrared-brightgalaxies among the widely separated pairs studied here. We find smallenhancements in far-IR activity in multiple galaxy systems relative toRBGS noninteracting galaxies with the same blue luminosity distribution.We also find no differences in infrared activity (as measured byinfrared color and luminosity) between late- and early-type spiralgalaxies.
| The IRAS Revised Bright Galaxy Sample
IRAS flux densities, redshifts, and infrared luminosities are reportedfor all sources identified in the IRAS Revised Bright Galaxy Sample(RBGS), a complete flux-limited survey of all extragalactic objects withtotal 60 μm flux density greater than 5.24 Jy, covering the entiresky surveyed by IRAS at Galactic latitudes |b|>5°. The RBGS includes629 objects, with median and mean sample redshifts of 0.0082 and 0.0126,respectively, and a maximum redshift of 0.0876. The RBGS supersedes theprevious two-part IRAS Bright Galaxy Samples(BGS1+BGS2), which were compiled before the final(Pass 3) calibration of the IRAS Level 1 Archive in 1990 May. The RBGSalso makes use of more accurate and consistent automated methods tomeasure the flux of objects with extended emission. The RBGS contains 39objects that were not present in the BGS1+BGS2,and 28 objects from the BGS1+BGS2 have beendropped from RBGS because their revised 60 μm flux densities are notgreater than 5.24 Jy. Comparison of revised flux measurements forsources in both surveys shows that most flux differences are in therange ~5%-25%, although some faint sources at 12 and 25 μm differ byas much as a factor of 2. Basic properties of the RBGS sources aresummarized, including estimated total infrared luminosities, as well asupdates to cross identifications with sources from optical galaxycatalogs established using the NASA/IPAC Extragalactic Database. Inaddition, an atlas of images from the Digitized Sky Survey with overlaysof the IRAS position uncertainty ellipse and annotated scale bars isprovided for ease in visualizing the optical morphology in context withthe angular and metric size of each object. The revised bolometricinfrared luminosity function, φ(Lir), forinfrared-bright galaxies in the local universe remains best fit by adouble power law, φ(L)~Lα, withα=-0.6(+/-0.1) and α=-2.2(+/-0.1) below and above the``characteristic'' infrared luminosityL*ir~1010.5Lsolar,respectively. A companion paper provides IRAS High Resolution (HIRES)processing of over 100 RBGS sources where improved spatial resolutionoften provides better IRAS source positions or allows for deconvolutionof close galaxy pairs.
| HYPERLEDA. II. The homogenized HI data
After a compilation of HI data from 611 references and new observationsmade in Nançay, we produce a catalog of homogenized HI data for16781 galaxies. The homogenization is made using the EPIDEMIC methodfrom which all data are progressively converted into the adoptedstandard. The result is a catalog giving: 1) the logarithm of twice themaximum rotation velocity, log 2V_Msin i, converted to thesystem of Mathewson et al. (\cite{Mathewson1996}). This quantity isgiven without correction for inclination; 2) the HI magnitude,m21, (area of the 21-cm line width expressed in magnitude)converted to the flux system of Theureau et al. (\cite{Theureau1998});3) the HI velocity, V_HI, expressed with the optical definition (i.e.,using wavelengths instead frequencies). The typical uncertainties are:0.04 for log 2V_Msin i, 0.25 mag for m21 and 9 kms-1 for V_HI.Full Tables \ref{epidemicw}, \ref{epidemicw2}, \ref{epidemicf},\ref{epidemicf2} and Fig. \ref{profiles} are available in electronicform at http://www.edpsciences.org. Full Tables \ref{references},\ref{cataf}, \ref{newdata} and \ref{notes} are available in electronicform at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/412/57
| A new catalogue of ISM content of normal galaxies
We have compiled a catalogue of the gas content for a sample of 1916galaxies, considered to be a fair representation of ``normality''. Thedefinition of a ``normal'' galaxy adopted in this work implies that wehave purposely excluded from the catalogue galaxies having distortedmorphology (such as interaction bridges, tails or lopsidedness) and/orany signature of peculiar kinematics (such as polar rings,counterrotating disks or other decoupled components). In contrast, wehave included systems hosting active galactic nuclei (AGN) in thecatalogue. This catalogue revises previous compendia on the ISM contentof galaxies published by \citet{bregman} and \citet{casoli}, andcompiles data available in the literature from several small samples ofgalaxies. Masses for warm dust, atomic and molecular gas, as well asX-ray luminosities have been converted to a uniform distance scale takenfrom the Catalogue of Principal Galaxies (PGC). We have used twodifferent normalization factors to explore the variation of the gascontent along the Hubble sequence: the blue luminosity (LB)and the square of linear diameter (D225). Ourcatalogue significantly improves the statistics of previous referencecatalogues and can be used in future studies to define a template ISMcontent for ``normal'' galaxies along the Hubble sequence. The cataloguecan be accessed on-line and is also available at the Centre desDonnées Stellaires (CDS).The catalogue is available in electronic form athttp://dipastro.pd.astro.it/galletta/ismcat and at the CDS via anonymousftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/405/5
| Arcsecond Positions of UGC Galaxies
We present accurate B1950 and J2000 positions for all confirmed galaxiesin the Uppsala General Catalog (UGC). The positions were measuredvisually from Digitized Sky Survey images with rms uncertaintiesσ<=[(1.2")2+(θ/100)2]1/2,where θ is the major-axis diameter. We compared each galaxymeasured with the original UGC description to ensure high reliability.The full position list is available in the electronic version only.
| Total magnitude, radius, colour indices, colour gradients and photometric type of galaxies
We present a catalogue of aperture photometry of galaxies, in UBVRI,assembled from three different origins: (i) an update of the catalogueof Buta et al. (1995) (ii) published photometric profiles and (iii)aperture photometry performed on CCD images. We explored different setsof growth curves to fit these data: (i) The Sersic law, (ii) The net ofgrowth curves used for the preparation of the RC3 and (iii) A linearinterpolation between the de Vaucouleurs (r(1/4) ) and exponential laws.Finally we adopted the latter solution. Fitting these growth curves, wederive (1) the total magnitude, (2) the effective radius, (3) the colourindices and (4) gradients and (5) the photometric type of 5169 galaxies.The photometric type is defined to statistically match the revisedmorphologic type and parametrizes the shape of the growth curve. It iscoded from -9, for very concentrated galaxies, to +10, for diffusegalaxies. Based in part on observations collected at the Haute-ProvenceObservatory.
| Search and Redshift Survey for IRAS Galaxies behind the Milky Way and Structure of the Local Void
This is the third and final paper of our systematic visual search forIRAS galaxies behind the Milky Way at |b| <= 15 deg. This paperpresents a catalog of 950 IRAS galaxies with 60 mu m flux densitieslarger than 0.6 Jy located between l = 0 deg and 150 deg, of which 293are newly identified by this search. We made a redshift survey for theidentified galaxies and obtained new redshift data of 171 galaxies. Wealso present newly measured redshifts of 27 IRAS galaxies between l =150 deg and 225 deg at |b| <= 15 deg. In this paper we studied thestructure of the Local void using IRAS galaxies and galaxies from theThird Reference Catalogue of Bright Galaxies in the region l = 30deg--120 deg and b = -50 deg to +30 deg. The center of the Local voidturned out to be located at l ~ 60 deg, b ~ -15 deg, and cz ~ 2500 kms-1, and the size is about 2500 km s-1 along the direction toward thecenter.
| The FCRAO Extragalactic CO Survey. I. The Data
Emission from the CO molecule at λ = 2.6 mm has been observed at1412 positions in 300 galaxies using the 14 m telescope of the FiveCollege Radio Astronomy Observatory (HPBW = 45"); these data comprisethe FCRAO Extragalactic CO Survey. In this paper we describe the galaxysample, present the data, and determine global CO fluxes and radialdistributions for the galaxies in the Survey. Future papers will dealwith the data analysis, both with regard to the global properties ofgalaxies and the radial distributions within them. CO emission wasdetected in 236 of the 300 Survey galaxies for an overall detection rateof 79%; among the 52 Sc galaxies in the Survey, the detection rate wasas high as 96%. most of the 193 galaxies observed in multiple positionsexhibit CO distributions which peak at the center. However, a smallnumber (10-primarily Sb galaxies) exhibit CO rings at 45" resolution,and a similar number (18-primarily Sc galaxies) have CO distributionswhich peak on one side of the center. We derive CO isophotal diametersfor 151 galaxies and find the mean ratio of CO to optical isophotaldiameters to be 0.5. We also find a trend along the Hubble sequence suchthat the mean ratio of CO to optical isophotal diameters is smallestamong the early-type spirals (SO/a, Sa, and Sab) and the mean ratioincreases for Sb, Sbc, and Sc galaxies, finally decreasing among thelater types. Comparison of the global fluxes we derive for the Surveygalaxies with independent measurements from the literature indicatesthat the global fluxes we derive are accurate to ~40%.
| The CO and HI emission of spiral and lenticular galaxies in the Fornax cluster.
We present a ^12^CO(1-0) and HI survey of the spirals and lenticulars inthe nearby southern cluster of galaxies Fornax. We have not found anyevidence for a strong HI deficiency in this cluster, which shows weakX-ray emission. However, three lenticular galaxies located near thecluster centre, NGC 1380, NGC 1386 and NGC 1387, present some HIdeficiency with an HI content respectively 50, 25 and 16 times timeslower than expected. On the other hand, the CO emission of Fornaxgalaxies is weak in general and we have clear detections of only 11galaxies out of 21 observed. We have found that on the average, lessthan 10 percent of the gas in these galaxies is in the molecular phase,if the CO to H_2_ conversion factor has the same value as in our galaxy.We have compared these results with those of other extragalactic surveysand found that such low H_2_ contents are characteristic of samples thatare not selected on a far-infrared criterion. In particular the nearbygalaxies surveyed by Sage (1993a, b) also have a low CO emission,although to a lesser level. The low molecular gas content of Fornaxgalaxies is consistent with their low star formation activity suggestedby their low far-infrared and nonthermal radiocontinuum emissions. Wehave made optical spectroscopical observations of the two CO-poorHI-rich spirals NGC 1350 and 1425 and have found that those galaxieshave weak Hα emission. We have also mapped the CO(1-0) and (2-1)emission of the interacting spiral NGC 1532. The CO distribution showstwo maxima at 7kpc radius, compatible with the presence of a molecularring. As most of Fornax spirals NGC 1532 is very poor in molecular gassince it contains about 30 times less H_2_ than HI.
| IRAS CPC Observations of Galaxies - Part One - Catalog and Atlas
. - We present the results of far-infrared imaging observations of 258regions of 12' x9' each centered on a selected individual galaxy, aclose pair, or a compact group of galaxies mapped at 50 and 100 micronwavelength with the CPC instrument of the IRAS satellite. The CPCinstrument has a significantly better resolution than the IRAS Surveyinstrument at these wavelengths, i.e. a round beam with a FWHM of about80" at 50 microns and 95" at 100 microns, respectively, intended to bematched to the diffraction limit of the telescope at 100 microns. Themaps were made using a new algorithm to correct for gain variations,which gives better results than the one used previously for the imagesmade available on tape in 1985. Of 262 objects observed, 167 and 188were detected at 50 and 100 microns, respectively, about 85% of thegalaxies from the same sample listed as detected by the Surveyinstrument in the IRAS Point Source Catalog. For all 55 galaxiesresolved (i.e. with a FWHM major axis diameter exceeding 1.6 times thebeam FWHM and/or extended lower-level emission) by the CPC we alsopresent the averaged maps at 50 and 100 microns. These 55 objectsinclude 35 for which there are no published maps obtained with the IRASSurvey instrument. We rescaled the flux densities of the published CPCmaps using the more accurate IRAS Survey instrument data, since theabsolute flux density calibration of the CPC is only accurate to about+/-60%. We also present images of a triplet of galaxies associated witha single Survey point source, which were resolved into separate sourcesby the CPC.
| Identifying galaxies in the zone of avoidance
A set of IR color criteria was applied to sources in the IRAS PointSource Catalog at low Galactic latitudes in order to select candidategalaxies. A total of 371 of the selected sources within a Galacticlatitude range (b) = 2-16 deg were searched for H I with the Arecibo 305m radio telescope. Twenty-six percent (97) were detected, including 36galaxies previously known only as IRAS sources. The H I spectra of thedetected galaxies are presented together with their observed redshiftsand velocity widths.
| Models for infrared emission from IRAS galaxies
The far-infrared spectra of galaxies detected in four wavelength bandsby IRAS have been modeled in terms of a cool disk component, a warmerstarburst component, and a Seyfert component peaking at 25 microns.Although the models are found to fit the observed spectra of non-Seyfertand several Seyfert galaxies, a more complex geometry for the dustdistribution is indicated for NGC 1068 and many other Seyfert galaxies.In some cases, the dust in the narrow-line region has a nonsphericallysymmetric geometry.
| A search for megamaser galaxies
The results of a search for OH megamaser emission from a sample of 32galaxies selected from the IRAS Point Source Catalog on the basis oftheir IR properties are presented. For each galaxy (other than those fewalready observed elsewhere), an optical redshift is obtained and both OHand H I emission are sought. The search yielded one new OH megamasergalaxy, and H I was detected toward nine objects. There are unlikely tobe any OH megamasers in the Southern Hemisphere with flux densitiescomparable to that of Arp 220 (280 mJy), although there may be apopulation of weaker megamasers. No special conditions are required toexplain the known OH megamasers other than those expected in a cool,dusty, active galaxy.
| Global properties of infrared bright galaxies
Infrared flux densities of 182 galaxies, including 50 galaxies in theVirgo cluster, were analyzed using IRAS data for 12, 25, 60, and 100microns, and the results were compared with data listed in the PointSource Catalog (PSC, 1985). In addition, IR luminosities, L(IRs),colors, and warm dust masses were derived for these galaxies and werecompared with the interstellar gas masses and optical luminosities ofthe galaxies. It was found that, for galaxies whose optical diametermeasures between 5 and 8 arcmin, the PSC flux densities areunderestimated by a factor of 2 at 60 microns, and by a factor of 1.5 at100 microns. It was also found that, for 49 galaxies, the mass of warmdust correlated well with the H2 mass, and that L(IR) correlated withL(H-alpha), demonstrating that the L(IR) measures the rate of starformation in these galaxies.
| Optical depth of molecular gas in starburst galaxies - Is M82 the prototype?
An attempt is made to survey the CO(2-1) emission toward the centers of17 IR-luminous galaxies which have previously been detected in CO(1-0).These galaxies span a wide range of size and L(FIR)/L(B) ratio, manyhave multiple-wavelength studies establishing them as starbursts, andsome bear a morphological resemblance to M 82. Nine galaxies aredetected and useful upper limits are placed on the remaining eight.Using the CO(2-1)/CO(1-0) ratio of antenna temperature as a diagnosticof optical depth, it is found that all of the galaxies containpredominantly optically thick molecular gas. This implies that the phaseof starburst during which the molecular gas is optically thin, currentlywitnessed in M 82, is either uncommon or short-lived.
| A further study of the relation of the radio-far-infrared in galaxies. I - Observations and data processing
The radio luminosities of 99 galaxies at 6.3 cm (and of 31 of them at2.8 cm) are determined on the basis of observations obtained with the100-m Effelsberg radio telescope during March-August 1984 and comparedto the IRAS color-corrected FIR luminosities, extending the survey of deJong et al. (1985). The data-reduction procedures are described, and theresults are presented in extensive tables and maps and brieflycharacterized. The correlation of radio to FIR luminosity is confirmedover about four decades in both parameters, and the dispersion of logP(6.3 cm)/L(FIR) is found to be about 0.2, which is significantlysmaller than the dispersion found by de Jong et al. The improvement isattributed to color correction, integration over the 100-60-micronrange, and the exclusion of ambiguous identifications.
| Molecular gas in high-luminosity IRAS galaxies
The paper reports observations of CO(J = 1-0) emission from an unbiasedsample of the highest-luminosity IRAS galaxies with the aim of measuringtheir molecular gas content and determining whether star formation is aviable energy source for these high luminosities. All of the observedgalaxies are rich in molecular gas with H2 masses in the range (4 x 10to the 9th)-(4 x 10 to the 10th) solar masses. Their primary luminositysource appears to be star formation in molecular clouds. The majority,if not all, of the most luminous IRAS galaxies (L-FIR greater than 10 tothe 11th solar luminosities) appear to be strongly interacting systems;those with the highest L-FIR/M(H2) ratios are mergers or close contactpairs.
| CO observations of infrared bright galaxies - The efficiency of star formation
CO emission has been detected in each of 14 of the IR-bright galaxieslisted in IRAS Circular 15; for the nine galaxies of the largest angularsize, the CO emission distributions along the major axis have beenmapped. A strong correlation is noted between total CO luminosities andIR ones for galaxies in each of three ranges of dust temperature. Theratio of IR/CO luminosities increases with the ratio of 60/100-micronflux densities, consistent with emission of thermal origin at thecharacteristic temperature given by the dust temperature. If thisluminosity ratio is a measure of the emergent stellar luminosity/unitmolecular mass, or the efficiency of star formation, this efficiencyvaries over almost two orders of magnitude from one galaxy to another.
| An Arecibo survey for extragalactic hydroxyl absorption. I - Presentation of results
Hydroxyl absorption has been detected in a total of 24 galaxies;megamaser emission in six additional galaxies brings the total number ofdetections of extragalactic OH to 30. About 50 percent of theextragalactic absorption lines are asymmetrically skewed toward the red,indicating that the molecular disks could have an unusual velocity orexcitation structure. The hyperfine ratio for the 1667 and 1665 MHztransitions in most galaxies lies within the limits specified by LTEconditions.
| Identification of infrared sources in the IRAS circulars
From IRAS (Infrared Astronomical Satellite) Circulars Nos. 4 to 15, 110infrared sources have been identified. Out of these 110 identifiedsources 99 are galaxies, nine are nebulae, one is a dark object, and oneis a non-stellar object. Thirty-five of these galaxies, have alreadybeen studied, mostly are spiral type. The characteristics of sixty-fourremaining galaxies, for which the type is not known or uncertain, arestudied by comparing their colors and luminosities with known galaxies.The galaxies observed by IRAS are mostly active galaxies.
| Properties of IRAS galaxies with B(0)T not greater than approximately 14.5
The optical and infrared properties of 86 galaxies from IRAS circulars1-15, identified with optically bright galaxies in RC-2 and UGC havebeen studied. It is seen that B(0)T, the face-on integratedblue magnitude, is correlated with the far-infrared (FIR) flux. For asubsample of 61 galaxies for which distances are available, it is foundthat the color temperature of FIR emitting dust is correlated with theFIR luminosity, but not with the blue band luminosity. This along withthe observed ratio of L(FIR)/L(B) implies that the observed blueluminosity is unlikely to be associated with young star formationactivity. Associating FIR luminosity with young star formation activityin molecular clouds and the blue luminosity to the mass of the galaxy, avalue of 5-10 solar luminosity/solar mass is estimated for the meanratio of total FIR luminosity to the mass of the gas in these galaxies.
| Strong H2O maser emission from the peculiar galaxy NGC 3079
The H2O laser emission detected from the peculiar galaxy NGC 3079,within 5 arcsec of the nucleus, has a total luminosity that (at about500 solar luminosities) distinguishes it as the most powerful maserdetected to date. Possible detection of a 200-solar luminosity H2O maseris noted in the distant interacting galaxy NGC 6240. Less luminous maseremission is confirmed towards NGC 1068, NGC 3034, and NGC 4258. H2O pumpmechanisms are discussed with a view to their ability to produce theluminosities observed.
| A radio continuum survey of nearby galaxies. I - Observations at 0.4, 0.8, 4.8, and 10.7 GHz
Observations have been conducted of a total of 136 galaxies at one ormore of four frequencies: 430, 834, 4750, and 10,700 MHz. For a subsetof these, spectral indices could be determined. A mean value alpha =-0.68 + or - 0.04 is found over the whole frequency range covered. Themean high frequency spectral index (4.9-10.7 GHz) for Sc galaxies isalpha = -0.55 + or - 0.07, which indicates the presence of significantamounts of thermal emission in a considerable fraction of the sample. At10.7 GHz the mean thermal contribution to the radio emission of thesample Sc galaxies is 35 + or - 15 percent; for the sample Sb galaxiesthis is 20 + or - 15 percent.
| 5-GHz survey of bright galaxies.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975AJ.....80..771S&db_key=AST
| Radio Observations of E and SO Galaxies
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970AJ.....75..523H&db_key=AST
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