1. Quenching of the star formation activity in cluster galaxies
A. Boselli et al 2016

2. Sample HRS (Herschel Reference Survey) Sample analysed
Volume-limited (15≤𝐷≤25 Mpc)
K-band-selected (2MASS 𝐾≤12 mag for LTG, 𝐾≤8.7 mag for ETG)
322 nearby galaxy
Sample analysed
168/260 for LTG
22/62 for ETG

3. Data photometric bands: FUV and NUV (GALEX) gri (SDSS) JHK (2MASS)
11 and 22 𝜇m (WISE)
100 and 160 𝜇m (PACS)
250, 350, 500 𝜇m (SPIRE)
H𝛼 imaging data

4. Data Spectroscopy: Atom and molecular gas data from Boselli+14
Age-sensitive absorption Balmer line indices have been extracted from the integrated medium-resolution (R ∼ 1000) spectra of the star-forming and quiescent galaxies of the HRS.
drifting the slit
GANDALF code to remove emission lines
Normalised using monochromatic g-band flux density
Atom and molecular gas data from Boselli+14
HI-deficiency: the difference in logarithmic scale between the expected and the observed HI mass of a galaxy of given angular size and morphological type
the rotational velocity

5. SED modelling
CIGALE produces synthetic UV to far-infrared SED of galaxies using different stellar population synthesis models available in the literature to trace the stellar emission and different dust models or empirical templates to trace the dust emission.
BC03 population synthesis models
Draine & Li 2007 physical models of dust emission:
𝑞 𝑃𝐴𝐻 : the fraction of the total dust mass in PAHs containing fewer than 10 3 atoms
𝑈 𝑚𝑖𝑛 : the intensity of the di use interstellar radiation field
𝛾 : the fraction of dust heated by young stars within photodissociation regions

6. Parametrisation of the star formation history
Buat+08, the star formation history of the multizone chemo-spectrophotometric models of galaxy evolution of Boissier & Prantzos (2000 ).
log 𝑆𝐹𝑅 𝑡 𝑠𝑒𝑐𝑢𝑙𝑎𝑟 =𝑎+𝑏 log 𝑡 +𝑐 𝑡 0.5
t: time elapsing after the first generation of stars are formed

7. Truncated SFH
QA: quenching age QF: quenching factor 𝑡 0 : age of the Universe at the present epoch

8. Spectral line indices 𝐻 𝛽 , 𝐻 𝛾 , 𝐻 𝛿
Transmissivity
𝐻 𝛽 , 𝐻 𝛾 , 𝐻 𝛿
CIGALE requires flux densities measured within a filter bandpass.
𝐻 𝛼 emission -> ionising photons -> pseudo-filter (LyC ) to characterise the ionising radiation

9. 1
Balmer line indices: 500Myrs
FUV and NUV: Myrs
H𝛼: <5Myrs

10. Mock catalogue of simulated galaxies
Test the solidity of this approach
simulated SED includes objects.
artificially introducing noise in the simulated SED according to the typical error
then fitted this simulated mock catalogue of SED and made a PDF analysis of the most critical variables.
Compare with Ciesla+16
Free parameter for SFH reduced from 3 to 2. (remove 𝜏 𝑚𝑎𝑖𝑛 , the typical timescale characterising the secular evolution of galaxies)
Use more age-sensitive photometric bands
a remarkable increase in the accuracy in the quenching parameters

11. rotational velocity is well measured
Whenever the truncation occurred at large QA and/or the QF is small, the imprints of these effects on the SED are hardly distinguishable from those due to possible variations in the secular evolution of galaxies.

12. Representative galaxy
NGC 4569

13. HRS
The model SED used in the following analysis were constructed using the appropriate rotational velocity as derived from kinematical data for each galaxy

14. Analysis the use of a truncated SFH increases the quality
Significantly in HI-deficient galaxies and QF high galaxies.

15. QF and QA QF increase with HI-def: QA (𝜌=0.48)
SFA is reduced when HI gas is removed
All ETG have QF=1
QA (𝜌=0.48)
For QF>0.5, more clear relationship
HI-def>0.8, QA∼1Gyr

16. QA=135 Myr for 0.5<QF<0.8
QA=235 Myr for QF>0.8
QA=1320 Myr for ETG

17. Identification of the perturbing mechanism
galaxy-galaxy interactions, galaxy harassment: timescale too long. Starvation: the effect of removing the outer galaxy halo would be to prevent further infall of gas into the disk, then the star formation would thus exhaust the available gas, quenching further star formation activity. Even if the process started ∼10Gyr ago, starvation would never be able to reduce the star formation activity of the perturbed galaxies by QF≥0.5.

19. Ram pressure stripping
Chemo-spectrophotometric models
ram-pressure-stripping efficiencies:
ϵ 0 =1.2 𝑀 ⊙ 𝑘𝑝 𝑐 −2 𝑦 𝑟 −1 : NGC4569
ϵ 0 =0.4 𝑀 ⊙ 𝑘𝑝 𝑐 −2 𝑦 𝑟 −1 : mean for Virgo cluster
The observed decrease in the star formation activity of HI-deficient galaxies in the main sequence relation can be explained by ram pressure stripping

20. For QF>0. 8 or HI-def>0
For QF>0.8 or HI-def>0.4 Both fraction drop by a factor of ∼5 from the core of the cluster(R<0.5) to the cluster periphery (R>4)

21. Rapid or slow environmental quenching?
Wetzel+13
First mildly declining on long timescale (2-4 Gyr)
Then a rapid decrease ( Gyr)
Timescale definition:
Our: the rapid decrease of the star formation activity that occurred when galaxies enter the rich Virgo cluster
Other: time since a galaxy became a satellite of a more massive halo.

22. Rapid or slow environmental quenching?
Quenching galaxies:
QF>0.5 or QF>0.8
Others: sSFR≤ 10 −11 𝑦 𝑟 −1
A rapid quenching of SFA of LTG that were recently accreted on the Virgo cluster, as predicted by ram-pressure-stripping models.

23. Conclusion