STAR FORMATION PROPERTIES IN THE LOCAL VOLUME GALAXIES VIA Hα AND FAR-ULTRAVIOLET FLUXES

Караченцев, И. Д.; Kaisina, E. I.

doi:10.1088/0004-6256/146/3/46

Cited by 99 publications

(84 citation statements)

References 55 publications

(55 reference statements)

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“…The Schmidt law, which has been found empirically and confirmed by many observations [22], relates the effective star formation rate observed in the galaxies and the surface density of gas in a power law dependence with an exponent of roughly 1.5. The integral rate of star formation and the hydrogen mass of the galaxies as a whole also follow this kind of dependence [23,10]. the relationship between the star formation rate and the neutral hydrogen mass in the Markarian galaxies.…”

Section: Some Integral Characteristics Of the Markarian Galaxiesmentioning

confidence: 89%

“…In an analysis of star formation in approximately 600 galaxies of the Local volume with measurements of H α and FUV fluxes, Karachentsev and Kaisina [23] noted the existence of an upper bound lim(logSSF R) = −9.4[yr −1 ] which encompasses all the galaxies within a volume of radius 10 Mpc. Karachentsev, et al [10], have determined the star formation rate of 520 especially isolated galaxies in the volume of the Local supercluster of radius ∼50 Mpc and also noticed the existence of this upper bound for logSSF R. This fact might seem trivial, since the evolution of isolated galaxies proceeds without significant tidal influence from neighbors, which provokes star formation outbursts.…”

Section: Discussionmentioning

confidence: 99%

“…The spiral galaxies occupy an intermediate position in the graph and the specific star formation rate is lowest for the galaxies with bulges. The upper limit corresponding to log(SSF R) = -9.4 for nearby isolated galaxies from the LOG catalog [10] and the galaxies from the nearby volume from [23] is indicated by a horizontal line. Only one galaxy, UGC 4499, within which Mrk 94 is identified with one of the knots in the spiral structure, lies above it.…”

Section: Specific and Effective Star Formation Ratesmentioning

confidence: 99%

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Star Formation Rates in Nearby Markarian Galaxies

2014

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The star formation rates for the 230 nearest Markarian galaxies with radial velocities VLG <3500 km/s have been determined from their far ultraviolet fluxes obtained with the GALEX satellite. We briefly discuss the observed relationship between the star formation rate and other integral parameters of these galaxies: stellar mass, hydrogen mass, morphological type, and activity index. On the average, the Markarian galaxies have reserves of gas that are a factor of two smaller than those of galaxies in the field of the same stellar mass and type. Despite their elevated activity, the specific rate of star formation in the Markarian galaxies, SF R/M * , does not exceed a limit of ∼dex(-9.4) [yr −1 ].

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Section: Some Integral Characteristics Of the Markarian Galaxiesmentioning

confidence: 89%

Section: Discussionmentioning

confidence: 99%

Section: Specific and Effective Star Formation Ratesmentioning

confidence: 99%

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Star Formation Rates in Nearby Markarian Galaxies

2014

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“…Figure 3 shows that this spread in X-ray luminosity from the CGM gas can explain the data. However, we should keep in mind that the spread in the data (Figure 4) can partly arise from the spread in the relation between SFR and galaxy dynamical mass, which is likely related to M * (Karachentsev & Kaisina 2013). We also note that the central SFR used in our models is an underestimation of a disk-wide SFR.…”

Section: Discussionmentioning

confidence: 86%

Diffuse X-Ray Emission From Star-Forming Galaxies

Sarkar

Nath

Sharma

et al. 2016

ApJL

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We study the diffuse X-ray luminosity (L X ) of star-forming galaxies using two-dimensional axisymmetric hydrodynamical simulations and analytical considerations of supernovae-(SNe-)driven galactic outflows. We find that the mass loading of the outflows, a crucial parameter for determining the X-ray luminosity, is constrained by the availability of gas in the central star-forming region, and a competition between cooling and expansion. We show that the allowed range of the mass loading factor can explain the observed scaling of L X with star formation rate (SFR) as µ L X SFR 2 for SFR  1  M yr −1 , and a flatter relation at low SFRs. We also show that the emission from the hot circumgalactic medium (CGM) in the halo of massive galaxies can explain the large scatter in the L SFR Xrelation for low SFRs (few  M yr −1 ). Our results suggest that galaxies with small SFRs and large diffuse X-ray luminosities are excellent candidates for the detection of the elusive CGM.

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“…In their study of X-ray emission from SNRs in the galaxy M83, Long et al (2014) estimated a surface area distribution of the SNRs to be approximately 1000 SNRs per square degree at a flux limit corresponding to that attained by our observation of NGC 45. For our source with the angular extent of NGC 45, we would expect to detect approximately 11 SNRs, but the SFR of M83 is an order of magnitude greater than that of NGC 45 (for example, Kaisinia 2013 and estimate the SFRs of NGC 45 and M83 to be 0.55 and 2.82 M  yr −1 , respectively, based on Hα fluxes of the galaxies). Assuming that the SNR detection rate of a galaxy scales in proportion to its SFR, from the estimate of Long et al (2014) we may expect to detect only one SNR in the X-ray in NGC 45, which broadly matches our result.…”

Section: Counterparts To Discrete X-ray Sources Detected At Other Wavmentioning

confidence: 93%

CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

Pannuti

Swartz²,

Laine

et al. 2015

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We present an analysis of high angular resolution observations made in the X-ray and the radio with the Chandra X-ray Observatory and the Karl Jansky Very Large Array (VLA), respectively, of the nearby spiral galaxy NGC 45. This galaxy is the third that we have considered in a study of the supernova remnant (SNR) populations of nearby spiral galaxies and the present work represents the first detailed analysis of the discrete X-ray and radio source populations of this galaxy. We analyzed data sets from the three pointed observations made of this galaxy with Chandra along with a merged data set obtained from combining these data sets: the total effective exposure time of the merged data set is 63515 s. A total of 25 discrete X-ray sources are found in the entire field of view of the ACIS-S3 chip, with 16 sources found within the visual extent of the galaxy. We estimate that as many as half of the sources detected in the entire field of view of the ACIS-S3 chip and seven of the sources detected in the optical extent of NGC 45 may be background sources. We analyzed the spectral properties of the discrete X-ray sources within the galaxy and conclude that the majority of these sources are X-ray binaries. We have searched for counterparts at different wavelengths to the discrete X-ray sources and we find two associations: one with a star cluster and the other with a background galaxy. We have found one source that is clearly variable within one observation and seven that are seen to vary from one observation to another. We also conduct a photometric analysis to determine the near-infrared fluxes of the discrete X-ray sources in Spitzer Infrared Array Camera channels. We constructed a cumulative luminosity function of the discrete X-ray sources seen toward NGC 45: taking into account simultaneously the luminosity function of background sources, the fitted slope of the cumulative luminosity function Γ = -1.3 1.6 0.7 -+ (all error bounds correspond to 90% confidence intervals). The VLA observations reveal seven discrete radio sources: we find no overlaps between these sources and the X-ray detected sources. Based on their measured spectral indices and their locations with respect to the visible extent of NGC 45, we classify one source as a candidate radio SNR associated with the galaxy and the others as likely background galaxies seen in projection toward NGC 45. Finally, we discuss the properties of a background cluster of galaxies (denoted as CXOU J001354.2-231254.7) seen in projection toward NGC 45 and detected by the Chandra observations. The fit parameters to the extracted Chandra spectra of this cluster are a column density N H = 0.07 (<0.14) × 10 22 cm −2 , a temperature kT = 4.22 1.42 2.08 -+ keV, an abundance Z = 0.30(<0.75) relative to solar and a redshift z = 0.28 ± 0.14. From the fit parameters we derive an electron number density n e = 4(±1) × 10 −3 cm −3 , an unabsorbed X-ray luminosity L 0.5 7.0 keV-8.77(±0.96) × 10 43 erg s −1 for the cluster and an X-ray emitting mass M = 2.32(±1.75) × 10 12 M  .

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STAR FORMATION PROPERTIES IN THE LOCAL VOLUME GALAXIES VIA Hα AND FAR-ULTRAVIOLET FLUXES

Cited by 99 publications

References 55 publications

Star Formation Rates in Nearby Markarian Galaxies

Star Formation Rates in Nearby Markarian Galaxies

Diffuse X-Ray Emission From Star-Forming Galaxies

CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

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