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Table 4.

Derived information for high-redshift quenched post-starburst and starburst systems, as introduced in Tables 1 and 2.

Galaxy ID z tSB tqui (c) τQ (e) τS τcool τdyn
/M⊙ yr−1 /Myr (a) /Myr (b) /Myr (d) /Myr (f) /Myr (g) /Myr
Quenched Post-Starbursts, High Redshift
A1689-zD1 7.60 4.9 350 81 −25.28 510 −27.07 540 76 13
UDF-983-964 7.6 290 170 −25.09 350 −27.43 390 100 26
GNS-zD2 10 240 250 −24.97 280 −27.09 330 120 15
MACS1149-JD1 9.11 11 100 290 −24.93 210 −27.68 250 43 23
CDFS-3225-4627 17 210 280 −24.74 180 −26.63 240 140 16
UDF-3244-4727 35 80 320 −24.43 80 −26.02 140 110 24
HDFN-3654-1216 36 190 430 −24.42 83 −26.86 230 130 38
GNS-zD3 38 110 350 −24.39 79 −26.11 160 140 22
UDF-640-1417 47 140 380 −24.30 67 −26.25 170 150 26
GNS-zD4 57 120 360 −24.22 57 −26.00 140 150 19
GNS-zD1 63 120 360 −24.17 59 −25.67 140 190 12
GNS-zD5 110 110 350 −23.93 40 −25.25 120 230 14
Starbursts, High Redshift
GN-z11 11.1 42* – −24.59 110 −25.07 120 110 11
EGS-zs8-1 7.73 100* – −24.08 34 −26.35 110 110 23
GN-108036 7.21 5.8* – −23.97 23 −25.30 120 51 61
SXDF-NB1006-2 7.21 1.0* – −23.43 6.4 −26.02 110 14 13

Notes. Columns for redshift z, star-formation rate during burst , length of starburst period tSB and dynamical timescale τdyn as shown previously and included here to aid comparisons between systems and timescales. This further introduces estimates for tqui, the time for which a post-starburst galaxy has remained relatively quiescent after its initial violent star-formation episode, heating rate via direct Coulomb CR heating in the interstellar medium of the host, ℋDC, heating rate via inverse-Compton X-ray heating of the inflowing filaments at an estimated average level, , estimated timescales for star-formation quenching τQ and strangulation τS, and cooling timescale for the inflowing gas, τcool.

(a)

Starburst time, tSB: estimated time over which the starburst phase has endured – asterisk * indicates starburst is still ongoing.

(b)

Quiescence timescale, tqui: estimated time over which the galaxy has maintained a low rate of star-formation, as determined from the age of the stellar population and starburst timescale. For our purposes, it is sufficient to estimate this as the stellar population ages, such that tqui ≈ τ* from Tables 1 and 2.

(c)

Coulomb heating rate, ℋDC: Decimal log of Coulomb heating rate in the interstellar medium responsible for cosmic ray quenching activity.

(d)

Quenching timescale, τQ: Quenching timescale, estimated from the virial temperature of the host galaxy.

(e)

Characteristic filament inverse-Compton heating rate, : Decimal log of the characteristic inverse-Compton X-ray heating rate in the filament structures, as responsible for strangulating star-formation.

(f)

Strangulation timescale τS: Strangulation timescale, estimated from the virial temperature of the inflowing filaments (not of the total system). This should be regarded as an upper limit, and is highly model-dependent.

(g)

Cooling timescale, τcool: Cooling timescale of the circumgalactic gases, being the minimum time required for star-formation to re-ignite after quenching or strangulation.

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