Context. Blue compact galaxies (BCG) are narrow emission-line systems that undergo a violent burs... more Context. Blue compact galaxies (BCG) are narrow emission-line systems that undergo a violent burst of star formation. They are compact, low-luminosity galaxies, with blue colors and low chemical abundances, which offer us a unique opportunity to investigate collective star formation and its effects on galaxy evolution in a relatively simple, dynamically unperturbed environment. Spatially resolved spectrophotometric studies of BCGs are essential for a better understanding of the role of starburst-driven feedback processes on the kinematical and chemical evolution of low-mass galaxies near and far. Aims. We carry out an integral field spectroscopy (IFS) study of a sample of luminous BCGs, with the aim to probe the morphology, kinematics, dust extinction, and excitation mechanisms of their warm interstellar medium (ISM). Methods. We obtained IFS data for five luminous BCGs with VIRUS-P, the prototype instrument for the Visible Integral Field Replicable Unit Spectrograph, attached to the 2.7 m Harlan J. Smith Telescope at the McDonald Observatory. VIRUS-P consists of a square array of 247 optical fibers, which covers a 109 × 109 field of view, with a spatial sampling of 4. 2 and a 0.3 filling factor. We observed in the 3550-5850 Å spectral range, with a resolution of 5 Å FWHM. From these data we built two-dimensional maps of the continuum and the most prominent emission-lines ([O ii] λ3727, Hγ, Hβ and [O iii] λ5007), and investigated the morphology of diagnostic emission-line ratios and the extinction patterns in the ISM as well as stellar and gas kinematics. Additionally, from integrated spectra we inferred total line fluxes and luminosity-weighted extinction coefficients and gas-phase metallicities. Results. All galaxies exhibit an overall regular morphology in the stellar continuum, while their warm ISM morphology is more complex: in II Zw 33 and Mrk 314, the star-forming regions are aligned along a chain-structure; Haro 1, NGC 4670 and III Zw 102 display several salient features, such as extended gaseous filaments and bubbles. A significant intrinsic absorption by dust is present in all galaxies, the most extreme case being III Zw 102. Our data reveal a plethora of kinematical patterns, from overall regular gas and stellar rotation to complex velocity fields produced by structurally and kinematically distinct components.
1 Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain e-m... more 1 Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain e-mail: bgarcia@iac.es 2 Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain 3 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands 4 Centro de Astrobiología (CSIC-INTA), Ctra. de Ajalvir, Km 4, 28850, Torrejón de Ardoz, Madrid, Spain 5 Department of Physics, Denys Wilkinson Building, Keble Road, University of Oxford, OX1 3RH, UK 6 Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain. 7 Institut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain.
In February 2004 the Cute-SCIDAR instrument was installed at the 1m Jacobus Kapteyn telescope (JK... more In February 2004 the Cute-SCIDAR instrument was installed at the 1m Jacobus Kapteyn telescope (JKT) for a systematic monitoring of the atmospheric turbulence at the Observatorio del Roque de los Muchachos (ORM). The proper knowledge of the atmospheric turbulence structure is crucial for optimising the efficiency of adaptive optics systems. SCIDAR has proved to be the most contrasted and efficient
Monthly Notices of the Royal Astronomical Society, 2008
We present new results on the nature of the Herbig-Haro-like object 73 (HHL 73, also known as [G8... more We present new results on the nature of the Herbig-Haro-like object 73 (HHL 73, also known as [G84b] 11) based on narrow-band CCD Hα and [S II] images of the HHL 73 field, and Integral Field Spectroscopy and radio continuum observations at 3.6 cm covering the emission of the HHL 73 object. The CCD images allow us to resolve the HHL 73 comet-shaped morphology into two components and a collimated emission feature of ∼ 4-arcsec long, reminiscent of a microjet. The IFS spectra of HHL 73 showed emission lines characteristic of the spectra of Herbig-Haro objects. The kinematics derived for HHL 73 are complex. The profiles of the [S II] λλ6717, 6731Å lines were well fitted with a model of three Gaussian velocity components peaking at V LSR ≃ −100, −20 and +35 km s −1. We found differences among the spatial distribution of the kinematic components that are compatible with the emission from a bipolar outflow with two blueshifted (low-and high-velocity) components. Extended radio continuum emission at 3.6 cm was detected showing a distribution in close agreement with the HHL 73 redshifted gas. From the results discussed here, we propose HHL 73 to be a true HH object. IRAS 21432+4719, offset 30 arcsec northeast from the HHL 73 apex, is the most plausible candidate to be driving HHL 73, although the evidence is not conclusive.
Monthly Notices of the Royal Astronomical Society, 2011
García-Lorenzo et al. presented a complete study of atmospheric parameters relevant for adaptive ... more García-Lorenzo et al. presented a complete study of atmospheric parameters relevant for adaptive optics in relation to wind speed at the Teide Observatory (Tenerife, Canary Islands, Spain). The atmospheric parameters were derived by combining C 2 N profiles derived from generalized-SCIDAR observations and wind vertical profiles from radiosondes. Later, Avila & Cuevas pointed out that the generalized-SCIDAR data processing leads an overstimation of the actual turbulence strength, showing that the error introduced strongly depends on the observational setup of the generalized-SCIDAR observations. Avila & Cuevas provided the exact expression of the error that can be applied to correct the retrieved C 2 N profiles. Recently, García-Lorenzo & Fuensalida calculated the error induced during data processing for all the observational configurations of the generalized-SCIDAR observations obtained at the Teide Observatory, showing that these errors are significant for some setups. Following the procedure in Avila & Cuevas, García-Lorenzo & Fuensalida corrected the full data base of atmospheric turbulence profiles for Teide Observatory. Here we present the corrected atmospheric parameters and show the different relationships between atmospheric parameters and wind speed. We conclude that the results of García-Lorenzo et al. were not drastically affected by the errors introduced in the C 2 N profiles in the generalized-SCIDAR data processing, and that the conclusions there are the same after the correction of the profiles and recalculation of the atmospheric parameters.
Monthly Notices of the Royal Astronomical Society, 2006
We describe a new method involving wavelet transforms for deriving the wind velocity associated w... more We describe a new method involving wavelet transforms for deriving the wind velocity associated with atmospheric turbulent layers from Generalized SCIDAR measurements. The algorithm analyses the cross-correlation of a series of scintillation patterns separated by lapses of t, 2 t, 3 t, 4 t and 5 t using wavelet transforms. Wavelet analysis provides the position, direction and altitude of the different turbulent layers detected in each cross-correlation. The comparison and consistency of the turbulent-layer displacements in consecutive crosscorrelations allow the determination of their velocities and avoid misidentifications associated with noise and/or overlapping layers. To validate the algorithm, we have compared the velocity of turbulent layers derived on four nights with the wind vertical profile provided by balloon measurements. The software is fully automated and is able to analyse huge amounts of Generalized SCIDAR measurements.
Proceedings of the International Astronomical Union, 2012
We have used the package CLOUDPROPS (Rosolowsky & Leroy 2008) in order to identify clouds, which ... more We have used the package CLOUDPROPS (Rosolowsky & Leroy 2008) in order to identify clouds, which are contained in data cubes of molecular/Hα line emission, and extract their properties. The molecular data cube is taken from the ALMA public archive and the ionized hydrogen data cube was obtained with the Fabry-Perot interferometer, GHαFaS, on the 4.2 m WHT in La Palma. In our study of the overlap region of the Antennae galaxies we have identified two populations of molecular clouds, above and below log M/M⊙ = 6.75 (in agreement with Wei et al. 2012 who find the break in mass at log M/M⊙ = 6.5) and two different populations of ionized gas clouds; the break in the luminosity occurs near log L = 37.6 (see Fig. 1). We have measured the masses, velocity dispersions and luminosities of the clouds, and derived relation between them for each population. Population II clouds (both molecular and ionized) tend to be located in the most luminous regions, while population I clouds can be found in...
Proceedings of the International Astronomical Union, 2012
We have observed Arp 270 using the GHαFaS Fabry-Perot spectrometer on the 4.2m William Herschel T... more We have observed Arp 270 using the GHαFaS Fabry-Perot spectrometer on the 4.2m William Herschel Telescope (La Palma). In the edge-on companion we detect a radial gas inflow of ∼ 0.36 M⊙/yr to the centre and also an axially confined outflow of ∼ 0.24 M⊙/yr from the nucleus in two opposing directions. We find two different behaviors between the physical properties of the HII regions. We suggest as a possible explanation a sub and supersonic regime.
We present preliminary results on the potential of HARMONI, the first light integral field spectr... more We present preliminary results on the potential of HARMONI, the first light integral field spectrograph for the ELT, to explore the evolution of central super massive black holes (SMBH)-host galaxy relation in the range from z∼0.7 to z∼2.5. We simulated HARMONI observations of QSO+host galaxy at different redshifts, assuming different morphologies for the host galaxy. As input, we combined MUSE observations of nearby galaxies and a theoretical QSO spectrum. These were dimmed and redshifted to the desired cosmic epoch. We scaled the total host galaxy luminosity to three different values, sampling three orders of magnitude. Likewise, we assumed two different luminosities for the central QSO. Simulations were performed for the 30×60 mas 2 HARMONI spatial scale and LTAO working at 0.67 arcsec seeing. The selected wavelength range (i.e., 4,700-5,300 Å at rest-frame) was sampled at the lowest HARMONI spectral resolving power (i.e., R∼3,200). This configuration included all the ingredients to estimate the host galaxy parameters and the SMBH mass, as well as for assessing the morphological type of the host galaxy.
Density waves in galaxy disks have been proposed over the years, in a variety of specific models,... more Density waves in galaxy disks have been proposed over the years, in a variety of specific models, to explain spiral arm structure and its relation to the mass distribution, notably in barred galaxies. An important parameter in dynamical density wave theories is the corotation radius, the galactocentric distance at which the stars and gas rotate at the same speed as the quasi-static propagating density wave. Determining corotation, and the pattern speed of a bar have become relevant to tests of cosmologically based theories of galaxy evolution involving the dynamical braking of bars by interaction with dark matter haloes. Here comparing two methods, one of which measures the pattern speed and the other the radius of corotation, using two instruments (an integral field spectrometer and a Fabry-Perot interferometer) and using both the stellar and interstellar velocity fields, we have determined the bar corotation radius, and three further radii of corotation for the SAB(s)b galaxy NGC3433. The results of both methods, with both instruments, and with both disk components give excellent agreement. This strengthens our confidence in the value of the two methods, and offers good perspectives for quantitative tests of different theoretical models.
Symposium - International Astronomical Union, 1999
We have obtained two-dimensional spectroscopy of the central ∼10″ × 12″ of the Wolf-Rayet galaxy ... more We have obtained two-dimensional spectroscopy of the central ∼10″ × 12″ of the Wolf-Rayet galaxy NGC 4861. We have carried out a preliminary analysis of the data, deriving continua at different wavelengths, and emission-line intensity maps (HeI λ4471, HeII λ4686, Hβ, [O III]λ4959, 5007) directly from the observed spectra.
Ground-based and Airborne Instrumentation for Astronomy VI, 2016
HARMONI is the E-ELT's first light visible and near-infrared integral field spectrograph. It will... more HARMONI is the E-ELT's first light visible and near-infrared integral field spectrograph. It will provide four different spatial scales, ranging from coarse spaxels of 60 × 30 mas best suited for seeing limited observations, to 4 mas spaxels that Nyquist sample the diffraction limited point spread function of the E-ELT at near-infrared wavelengths. Each spaxel scale may be combined with eleven spectral settings, that provide a range of spectral resolving powers (R ~3500, 7500 and 20000) and instantaneous wavelength coverage spanning the 0.5-2.4 μm wavelength range of the instrument. In autumn 2015, the HARMONI project started the Preliminary Design Phase, following signature of the contract to design, build, test and commission the instrument, signed between the European Southern Observatory and the UK Science and Technology Facilities Council. Crucially, the contract also includes the preliminary design of the HARMONI Laser Tomographic Adaptive Optics system. The instrument's technical specifications were finalized in the period leading up to contract signature. In this paper, we report on the first activity carried out during preliminary design, defining the baseline architecture for the system, and the trade-off studies leading up to the choice of baseline.
Optics in Atmospheric Propagation and Adaptive Systems XII, 2009
The development of adaptive optics systems for projects related to large telescopes demands a pro... more The development of adaptive optics systems for projects related to large telescopes demands a proper knowledge of the atmospheric turbulence. Due to the lack of long-term information on optical turbulence, high-altitude winds (in particular winds at the 200-mbar pressure level) were adopted as a parameter for estimating the total turbulence at a particular site, since there are large wind databases
Starbursts are events in which hundreds of solar masses per year of gas are transformed into star... more Starbursts are events in which hundreds of solar masses per year of gas are transformed into stars on timescales much shorter than the Hubble time. They are essential in galaxy evolution as they are responsible for the largest part of the chemically enriched material in the interstellar and intergalactic medium where the metals have been deposited through stellar and supergalactic
Context. Blue compact galaxies (BCG) are narrow emission-line systems that undergo a violent burs... more Context. Blue compact galaxies (BCG) are narrow emission-line systems that undergo a violent burst of star formation. They are compact, low-luminosity galaxies, with blue colors and low chemical abundances, which offer us a unique opportunity to investigate collective star formation and its effects on galaxy evolution in a relatively simple, dynamically unperturbed environment. Spatially resolved spectrophotometric studies of BCGs are essential for a better understanding of the role of starburst-driven feedback processes on the kinematical and chemical evolution of low-mass galaxies near and far. Aims. We carry out an integral field spectroscopy (IFS) study of a sample of luminous BCGs, with the aim to probe the morphology, kinematics, dust extinction, and excitation mechanisms of their warm interstellar medium (ISM). Methods. We obtained IFS data for five luminous BCGs with VIRUS-P, the prototype instrument for the Visible Integral Field Replicable Unit Spectrograph, attached to the 2.7 m Harlan J. Smith Telescope at the McDonald Observatory. VIRUS-P consists of a square array of 247 optical fibers, which covers a 109 × 109 field of view, with a spatial sampling of 4. 2 and a 0.3 filling factor. We observed in the 3550-5850 Å spectral range, with a resolution of 5 Å FWHM. From these data we built two-dimensional maps of the continuum and the most prominent emission-lines ([O ii] λ3727, Hγ, Hβ and [O iii] λ5007), and investigated the morphology of diagnostic emission-line ratios and the extinction patterns in the ISM as well as stellar and gas kinematics. Additionally, from integrated spectra we inferred total line fluxes and luminosity-weighted extinction coefficients and gas-phase metallicities. Results. All galaxies exhibit an overall regular morphology in the stellar continuum, while their warm ISM morphology is more complex: in II Zw 33 and Mrk 314, the star-forming regions are aligned along a chain-structure; Haro 1, NGC 4670 and III Zw 102 display several salient features, such as extended gaseous filaments and bubbles. A significant intrinsic absorption by dust is present in all galaxies, the most extreme case being III Zw 102. Our data reveal a plethora of kinematical patterns, from overall regular gas and stellar rotation to complex velocity fields produced by structurally and kinematically distinct components.
1 Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain e-m... more 1 Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain e-mail: bgarcia@iac.es 2 Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain 3 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands 4 Centro de Astrobiología (CSIC-INTA), Ctra. de Ajalvir, Km 4, 28850, Torrejón de Ardoz, Madrid, Spain 5 Department of Physics, Denys Wilkinson Building, Keble Road, University of Oxford, OX1 3RH, UK 6 Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain. 7 Institut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain.
In February 2004 the Cute-SCIDAR instrument was installed at the 1m Jacobus Kapteyn telescope (JK... more In February 2004 the Cute-SCIDAR instrument was installed at the 1m Jacobus Kapteyn telescope (JKT) for a systematic monitoring of the atmospheric turbulence at the Observatorio del Roque de los Muchachos (ORM). The proper knowledge of the atmospheric turbulence structure is crucial for optimising the efficiency of adaptive optics systems. SCIDAR has proved to be the most contrasted and efficient
Monthly Notices of the Royal Astronomical Society, 2008
We present new results on the nature of the Herbig-Haro-like object 73 (HHL 73, also known as [G8... more We present new results on the nature of the Herbig-Haro-like object 73 (HHL 73, also known as [G84b] 11) based on narrow-band CCD Hα and [S II] images of the HHL 73 field, and Integral Field Spectroscopy and radio continuum observations at 3.6 cm covering the emission of the HHL 73 object. The CCD images allow us to resolve the HHL 73 comet-shaped morphology into two components and a collimated emission feature of ∼ 4-arcsec long, reminiscent of a microjet. The IFS spectra of HHL 73 showed emission lines characteristic of the spectra of Herbig-Haro objects. The kinematics derived for HHL 73 are complex. The profiles of the [S II] λλ6717, 6731Å lines were well fitted with a model of three Gaussian velocity components peaking at V LSR ≃ −100, −20 and +35 km s −1. We found differences among the spatial distribution of the kinematic components that are compatible with the emission from a bipolar outflow with two blueshifted (low-and high-velocity) components. Extended radio continuum emission at 3.6 cm was detected showing a distribution in close agreement with the HHL 73 redshifted gas. From the results discussed here, we propose HHL 73 to be a true HH object. IRAS 21432+4719, offset 30 arcsec northeast from the HHL 73 apex, is the most plausible candidate to be driving HHL 73, although the evidence is not conclusive.
Monthly Notices of the Royal Astronomical Society, 2011
García-Lorenzo et al. presented a complete study of atmospheric parameters relevant for adaptive ... more García-Lorenzo et al. presented a complete study of atmospheric parameters relevant for adaptive optics in relation to wind speed at the Teide Observatory (Tenerife, Canary Islands, Spain). The atmospheric parameters were derived by combining C 2 N profiles derived from generalized-SCIDAR observations and wind vertical profiles from radiosondes. Later, Avila & Cuevas pointed out that the generalized-SCIDAR data processing leads an overstimation of the actual turbulence strength, showing that the error introduced strongly depends on the observational setup of the generalized-SCIDAR observations. Avila & Cuevas provided the exact expression of the error that can be applied to correct the retrieved C 2 N profiles. Recently, García-Lorenzo & Fuensalida calculated the error induced during data processing for all the observational configurations of the generalized-SCIDAR observations obtained at the Teide Observatory, showing that these errors are significant for some setups. Following the procedure in Avila & Cuevas, García-Lorenzo & Fuensalida corrected the full data base of atmospheric turbulence profiles for Teide Observatory. Here we present the corrected atmospheric parameters and show the different relationships between atmospheric parameters and wind speed. We conclude that the results of García-Lorenzo et al. were not drastically affected by the errors introduced in the C 2 N profiles in the generalized-SCIDAR data processing, and that the conclusions there are the same after the correction of the profiles and recalculation of the atmospheric parameters.
Monthly Notices of the Royal Astronomical Society, 2006
We describe a new method involving wavelet transforms for deriving the wind velocity associated w... more We describe a new method involving wavelet transforms for deriving the wind velocity associated with atmospheric turbulent layers from Generalized SCIDAR measurements. The algorithm analyses the cross-correlation of a series of scintillation patterns separated by lapses of t, 2 t, 3 t, 4 t and 5 t using wavelet transforms. Wavelet analysis provides the position, direction and altitude of the different turbulent layers detected in each cross-correlation. The comparison and consistency of the turbulent-layer displacements in consecutive crosscorrelations allow the determination of their velocities and avoid misidentifications associated with noise and/or overlapping layers. To validate the algorithm, we have compared the velocity of turbulent layers derived on four nights with the wind vertical profile provided by balloon measurements. The software is fully automated and is able to analyse huge amounts of Generalized SCIDAR measurements.
Proceedings of the International Astronomical Union, 2012
We have used the package CLOUDPROPS (Rosolowsky & Leroy 2008) in order to identify clouds, which ... more We have used the package CLOUDPROPS (Rosolowsky & Leroy 2008) in order to identify clouds, which are contained in data cubes of molecular/Hα line emission, and extract their properties. The molecular data cube is taken from the ALMA public archive and the ionized hydrogen data cube was obtained with the Fabry-Perot interferometer, GHαFaS, on the 4.2 m WHT in La Palma. In our study of the overlap region of the Antennae galaxies we have identified two populations of molecular clouds, above and below log M/M⊙ = 6.75 (in agreement with Wei et al. 2012 who find the break in mass at log M/M⊙ = 6.5) and two different populations of ionized gas clouds; the break in the luminosity occurs near log L = 37.6 (see Fig. 1). We have measured the masses, velocity dispersions and luminosities of the clouds, and derived relation between them for each population. Population II clouds (both molecular and ionized) tend to be located in the most luminous regions, while population I clouds can be found in...
Proceedings of the International Astronomical Union, 2012
We have observed Arp 270 using the GHαFaS Fabry-Perot spectrometer on the 4.2m William Herschel T... more We have observed Arp 270 using the GHαFaS Fabry-Perot spectrometer on the 4.2m William Herschel Telescope (La Palma). In the edge-on companion we detect a radial gas inflow of ∼ 0.36 M⊙/yr to the centre and also an axially confined outflow of ∼ 0.24 M⊙/yr from the nucleus in two opposing directions. We find two different behaviors between the physical properties of the HII regions. We suggest as a possible explanation a sub and supersonic regime.
We present preliminary results on the potential of HARMONI, the first light integral field spectr... more We present preliminary results on the potential of HARMONI, the first light integral field spectrograph for the ELT, to explore the evolution of central super massive black holes (SMBH)-host galaxy relation in the range from z∼0.7 to z∼2.5. We simulated HARMONI observations of QSO+host galaxy at different redshifts, assuming different morphologies for the host galaxy. As input, we combined MUSE observations of nearby galaxies and a theoretical QSO spectrum. These were dimmed and redshifted to the desired cosmic epoch. We scaled the total host galaxy luminosity to three different values, sampling three orders of magnitude. Likewise, we assumed two different luminosities for the central QSO. Simulations were performed for the 30×60 mas 2 HARMONI spatial scale and LTAO working at 0.67 arcsec seeing. The selected wavelength range (i.e., 4,700-5,300 Å at rest-frame) was sampled at the lowest HARMONI spectral resolving power (i.e., R∼3,200). This configuration included all the ingredients to estimate the host galaxy parameters and the SMBH mass, as well as for assessing the morphological type of the host galaxy.
Density waves in galaxy disks have been proposed over the years, in a variety of specific models,... more Density waves in galaxy disks have been proposed over the years, in a variety of specific models, to explain spiral arm structure and its relation to the mass distribution, notably in barred galaxies. An important parameter in dynamical density wave theories is the corotation radius, the galactocentric distance at which the stars and gas rotate at the same speed as the quasi-static propagating density wave. Determining corotation, and the pattern speed of a bar have become relevant to tests of cosmologically based theories of galaxy evolution involving the dynamical braking of bars by interaction with dark matter haloes. Here comparing two methods, one of which measures the pattern speed and the other the radius of corotation, using two instruments (an integral field spectrometer and a Fabry-Perot interferometer) and using both the stellar and interstellar velocity fields, we have determined the bar corotation radius, and three further radii of corotation for the SAB(s)b galaxy NGC3433. The results of both methods, with both instruments, and with both disk components give excellent agreement. This strengthens our confidence in the value of the two methods, and offers good perspectives for quantitative tests of different theoretical models.
Symposium - International Astronomical Union, 1999
We have obtained two-dimensional spectroscopy of the central ∼10″ × 12″ of the Wolf-Rayet galaxy ... more We have obtained two-dimensional spectroscopy of the central ∼10″ × 12″ of the Wolf-Rayet galaxy NGC 4861. We have carried out a preliminary analysis of the data, deriving continua at different wavelengths, and emission-line intensity maps (HeI λ4471, HeII λ4686, Hβ, [O III]λ4959, 5007) directly from the observed spectra.
Ground-based and Airborne Instrumentation for Astronomy VI, 2016
HARMONI is the E-ELT's first light visible and near-infrared integral field spectrograph. It will... more HARMONI is the E-ELT's first light visible and near-infrared integral field spectrograph. It will provide four different spatial scales, ranging from coarse spaxels of 60 × 30 mas best suited for seeing limited observations, to 4 mas spaxels that Nyquist sample the diffraction limited point spread function of the E-ELT at near-infrared wavelengths. Each spaxel scale may be combined with eleven spectral settings, that provide a range of spectral resolving powers (R ~3500, 7500 and 20000) and instantaneous wavelength coverage spanning the 0.5-2.4 μm wavelength range of the instrument. In autumn 2015, the HARMONI project started the Preliminary Design Phase, following signature of the contract to design, build, test and commission the instrument, signed between the European Southern Observatory and the UK Science and Technology Facilities Council. Crucially, the contract also includes the preliminary design of the HARMONI Laser Tomographic Adaptive Optics system. The instrument's technical specifications were finalized in the period leading up to contract signature. In this paper, we report on the first activity carried out during preliminary design, defining the baseline architecture for the system, and the trade-off studies leading up to the choice of baseline.
Optics in Atmospheric Propagation and Adaptive Systems XII, 2009
The development of adaptive optics systems for projects related to large telescopes demands a pro... more The development of adaptive optics systems for projects related to large telescopes demands a proper knowledge of the atmospheric turbulence. Due to the lack of long-term information on optical turbulence, high-altitude winds (in particular winds at the 200-mbar pressure level) were adopted as a parameter for estimating the total turbulence at a particular site, since there are large wind databases
Starbursts are events in which hundreds of solar masses per year of gas are transformed into star... more Starbursts are events in which hundreds of solar masses per year of gas are transformed into stars on timescales much shorter than the Hubble time. They are essential in galaxy evolution as they are responsible for the largest part of the chemically enriched material in the interstellar and intergalactic medium where the metals have been deposited through stellar and supergalactic
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Papers by Begona Lorenzo